{"instruction": "what is the prompt that generates the input?", "input": "Based on the SDSS catalog, we have found new close quasar-galaxy pairs.Quasars projected onto the halos of nearer galaxies are encountered among themultitude of quasars observed at various distances from us. Among them thereare quasars that are close to the galaxies not only in angular separation, butalso in redshift. Such quasar-galaxy pairs are called close pairs. We developedfurther the hypothesis that such pairs appear, because the fluxer on thenucleus of the more distant galaxy passes through halo globular clusters of thenearer galaxy,resulting in magnification and splitting of the image of thesource that we interpret as a quasar. To corroborate this hypothesis, weanalyzed the distribution of quasars in the plane of the halos of thesegalaxies. The quasars from close pairs were found to follow the density profileof globular clusters in the halos of elliptical and spiral galaxies with slopesof -1.5 and -2.4 for elliptical and spiral galaxies, respectively. Thissuggests that quasars do not appear near galaxies by chance and that quasarsare associated with galaxies via halo globular clusters.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We propose a combined experimental (Atomic Force Microscopy) and theoreticalstudy of the structural and dynamical properties of nucleosomes. In contrast tobiochemical approaches, this method allows to determine simultaneously the DNAcomplexed length distribution and nucleosome position in various contexts.First, we show that differences in the nucleo-proteic structure observedbetween conventional H2A and H2A.Bbd variant nucleosomes induce quantitativechanges in the in the length distribution of DNA complexed with histones. Then,the sliding action of remodeling complex SWI/SNF is characterized through theevolution of the nucleosome position and wrapped DNA length mapping. Using alinear energetic model for the distribution of DNA complexed length, we extractthe net wrapping energy of DNA onto the histone octamer, and compare it toprevious studies.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present semi-analytical constraint on the amount of dark matter in themerging bullet galaxy cluster using the classical Local Group timing arguments.We consider particle orbits in potential models which fit the lensing data.{\\it Marginally consistent} CDM models in Newtonian gravity are found with atotal mass M_{CDM} = 1 x 10^{15}Msun of Cold DM: the bullet subhalo can movewith V_{DM}=3000km/s, and the \"bullet\" X-ray gas can move withV_{gas}=4200km/s. These are nearly the {\\it maximum speeds} that areaccelerable by the gravity of two truncated CDM halos in a Hubble time evenwithout the ram pressure. Consistency breaks down if one adopts higher end ofthe error bars for the bullet gas speed (5000-5400km/s), and the bullet gaswould not be bound by the sub-cluster halo for the Hubble time. Models withV_{DM}~ 4500km/s ~ V_{gas} would invoke unrealistic large amount M_{CDM}=7x10^{15}Msun of CDM for a cluster containing only ~ 10^{14}Msun of gas. Ourresults are generalisable beyond General Relativity, e.g., a speed of$4500\\kms$ is easily obtained in the relativistic MONDian lensing model ofAngus et al. (2007). However, MONDian model with little hot dark matter$M_{HDM} \\le 0.6\\times 10^{15}\\msun$ and CDM model with a small halo mass $\\le1\\times 10^{15}\\msun$ are barely consistent with lensing and velocity data.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Using a general Ginzburg-Landau effective Lagrangian, we study thetopological structure and low-lying collective modes of dense QCD having bothchiral and diquark condensates, for two and three massless flavors. As we foundearlier, the QCD axial anomaly acts as an external field applied to the chiralcondensate in a color superconductor and, as a new critical point emerges,leads to a crossover between the broken chiral symmetry and colorsuperconducting phases. At intermediate densities where both chiral and diquarkcondensates are present, we derive a generalized Gell-Mann- Oakes-Rennerrelation between the masses of pseudoscalar bosons and the magnitude of thechiral and diquark-condensates. We show explicitly the continuity of theordinary pion at low densities to a generalized pion at high densities.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "HD 52265 is the only known exoplanet-host star selected as a main target forthe seismology programme of the CoRoT satellite. As such, it will be observedcontinuously during five months, which is of particular interest in theframework of planetary systems studies. This star was misclassified as a giantin the Bright Star Catalog, while it is more probably on the main-sequence orat the beginning of the subgiant branch. We performed an extensive analysis ofthis star, showing how asteroseismology may lead to a precise determination ofits external parameters and internal structure. We first reviewed theobservational constraints on the metallicity, the gravity and the effectivetemperature derived from the spectroscopic observations of HD 52265. We alsoderived its luminosity using the Hipparcos parallax. We computed theevolutionary tracks for models of various metallicities which cross therelevant observational error boxes in the gravity-effective temperature plane.We selected eight different stellar models which satisfy the observationalconstraints, computed their p-modes frequencies and analysed specific seismictests. The possible models for HD 52265, which satisfy the constraints derivedfrom the spectroscopic observations, are different in both their external andinternal parameters. They lie either on the main sequence or at the beginningof the subgiant branch. The differences in the models lead to quite differentproperties of their oscillation frequencies. We give evidences of aninteresting specific behaviour of these frequencies in case of helium-richcores: the ``small separations'' may become negative and give constraints onthe size of the core. We expect that the observations of this star by the CoRoTsatellite wi ll allow choosing between these possible models.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The emergence of magnetic flux from the convection zone into the corona is animportant process for the dynamical evolution of the coronal magnetic field. Inthis paper we extend our previous numerical investigations, by looking at theprocess of flux interaction as an initially twisted flux tube emerges into aplane parallel, coronal magnetic field. Significant differences are found inthe dynamical appearance and evolution of the emergence process depending onthe relative orientation between the rising flux system and any preexistingcoronal field. When the flux systems are nearly anti-parallel, the experimentsshow substantial reconnection and demonstrate clear signatures of a hightemperature plasma located in the high velocity outflow regions extending fromthe reconnection region. However, the cases that have a more parallelorientation of the flux systems show very limited reconnection and none of theassociated features. Despite the very different amount of reconnection betweenthe two flux systems, it is found that the emerging flux that is stillconnected to the original tube, reaches the same height as a function of time.As a compensation for the loss of tube flux, a clear difference is found in theextent of the emerging loop in the direction perpendicular to the main axis ofthe initial flux tube. Increasing amounts of magnetic reconnection decrease thevolume, which confines the remaining tube flux.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "In most theories of gravity involving torsion, the source for torsion is theintrinsic spin of matter. Since the spins of fermions are normally randomlyoriented in macroscopic bodies, the torsion generated is normally negligible.However, in a recent paper, Mao et al. point out that there is a class oftheories in which the angular momentum of macroscopic spinning bodies generatesa significant amount of torsion. They argue that by the principle of actionequals reaction, one would expect the angular momentum of test bodies to coupleto a background torsion field, and therefore the precession of the GPBgyroscopes should be affected in these theories by the torsion generated by theEarth. We show that in fact the principle of action equals reaction does notapply to these theories. We examine in detail a generalization of theHayashi-Shirafuji theory suggested by Mao et al. calledEinstein-Hayashi-Shirafuji theory. There are a variety of different versions ofthis theory, depending on the precise form of the coupling to matter chosen forthe torsion. We show that for any coupling to matter that is compatible withthe spin transport equation postulated by Mao et al., the theory has eitherghosts or an ill-posed initial value formulation. These theoretical problemscan be avoided by specializing the parameters of the theory and in additionchoosing the standard minimal coupling to matter of the torsion tensor. Thisyields a consistent theory, but one in which the action equals reactionprinciple is violated, and in which the angular momentum of the gyroscopes doesnot couple to the Earth's torsion field. Thus, the Einstein-Hayashi-Shirafujitheory does not predict a detectable torsion signal for Gravity Probe B. Theremay be other torsion theories which do.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Bi-intuitionistic logic is the extension of intuitionistic logic with aconnective dual to implication. Bi-intuitionistic logic was introduced byRauszer as a Hilbert calculus with algebraic and Kripke semantics. But hersubsequent ``cut-free'' sequent calculus for BiInt has recently been shown byUustalu to fail cut-elimination. We present a new cut-free sequent calculus forBiInt, and prove it sound and complete with respect to its Kripke semantics.Ensuring completeness is complicated by the interaction between implication andits dual, similarly to future and past modalities in tense logic. Our calculushandles this interaction using extended sequents which pass information frompremises to conclusions using variables instantiated at the leaves of failedderivation trees. Our simple termination argument allows our calculus to beused for automated deduction, although this is not its main purpose.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present results from a high-angular-resolution survey of 78 very low mass(VLM) binary systems with 6.0 <= V-K colour <= 7.5 and proper motion >= 0.15arcsec/yr. 21 VLM binaries were detected, 13 of them new discoveries. The newbinary systems range in separation between 0.18 arcsec and 1.3 arcsec. Thedistance-corrected binary fraction is 13.5% (+6.5%/-4%), in agreement withprevious results. 9 of the new binary systems have orbital radii > 10 AU,including a new wide VLM binary with 27 AU projected orbital separation. One ofthe new systems forms two components of a 2300 AU separation triple system. Wefind that the orbital radius distribution of the binaries with V-K < 6.5 inthis survey appears to be different from that of redder (lower-mass) objects,suggesting a possible rapid change in the orbital radius distribution at aroundthe M5 spectral type. The target sample was also selected to investigate X-rayactivity among VLM binaries. There is no detectable correlation between excessX-Ray emission and the frequency and binary properties of the VLM systems.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "This paper examines the effect of temperature on the structural stability andmechanical properties of 20 layered (10,10) single walled carbon nanotubes(SWCNTs) under tensile loading using an O(N) tight binding molecular dynamics(TBMD) simulation method. We observed that (10,10) tube can sustain itsstructural stability for the strain values of 0.23 in elongation and 0.06 incompression at 300K. Bond breaking strain value decreases with increasingtemperature under streching but not under compression. The elastic limit,Young's modulus, tensile strength and Poisson ratio are calculated as 0.10,0.395 TPa, 83.23 GPa, 0.285, respectively, at 300K. In the temperature rangefrom 300K to 900K; Young's modulus and the tensile strengths are decreasingwith increasing temperature while the Poisson ratio is increasing. At highertemperatures, Young's modulus starts to increase while the Poisson ratio andtensile strength decrease. In the temperature range from 1200K to 1800K, theSWCNT is already deformed and softened. Applying strain on these deformed andsoftened SWCNTs do not follow the same pattern as in the temperature range of300K to 900K.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "(Abridged) We present numerical hydrodynamical simulations of the formation,evolution and gravitational collapse of isothermal molecular cloud cores. Acompressive wave is set up in a constant sub-Jeans density distribution ofradius r = 1 pc. As the wave travels through the simulation grid, ashock-bounded spherical shell is formed. The inner shock of this shell reachesand bounces off the center, leaving behind a central core with an initiallyalmost uniform density distribution, surrounded by an envelope consisting ofthe material in the shock-bounded shell, with a power-law density profile thatat late times approaches a logarithmic slope of -2 even in non-collapsingcases. The resulting density structure resembles a quiescent core of radius <0.1 pc, with a Bonnor-Ebert-like (BE-like) profile, although it has significantdynamical differences: it is initially non-self-gravitating and confined by theram pressure of the infalling material, and consequently, growing continuouslyin mass and size. With the appropriate parameters, the core mass eventuallyreaches an effective Jeans mass, at which time the core begins to collapse.Thus, there is necessarily a time delay between the appearance of the core andthe onset of its collapse, but this is not due to the dissipation of itsinternal turbulence as it is often believed. These results suggest thatpre-stellar cores may approximate Bonnor-Ebert structures which are however ofvariable mass and may or may not experience gravitational collapse, inqualitative agreement with the large observed frequency of cores with BE-likeprofiles.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "On the basis of the extensive air shower (EAS) data obtained by the GAMMAexperiment, the energy spectra and elemental composition of the primary cosmicrays are derived in the 1-100 PeV energy range. The reconstruction of theprimary energy spectra is carried out using an EAS inverse approach in theframework of the SIBYLL2.1 and QGSJET01 interaction models and the hypothesisof power-law primary energy spectra with rigidity-dependent knees. The energyspectra of primary H, He, O-like and Fe-like nuclei obtained with the SIBYLLinteraction model agree with corresponding extrapolations of the balloon andsatellite data to ~1 PeV energies. The energy spectra obtained from the QGSJETmodel show a predominantly proton composition in the knee region. Therigidity-dependent knee feature of the primary energy spectra for eachinteraction model is displayed at the following rigidities: ~2.5+/-0.2 PV(SIBYLL) and ~3.1-4.2 PV (QGSJET). All the results presented are derived takinginto account the detector response, the reconstruction uncertainties of the EASparameters, and fluctuations in the EAS development.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "In this talk we discuss at hand of two examples the crucial role played byself consistency in hadron physics. The first example concerns the quark-massdependence of the baryon octet and decuplet masses. It is shown that within aself consistent one-loop approach based on the chiral Lagrangian the'mysterious' quark-mass dependence of the $\\Xi$ mass predicted by the MILCcollaboration may be recovered in terms of a discontinuous chiralextrapolation. This is a consequence of self consistency imposed on the partialsummation, i.e. the masses used in the loop functions are identical to thoseobtained from the baryon self energies. In the second example we discuss recentstudies on the properties of D mesons in cold nuclear matter as they arepredicted by coupled-channel dynamics. Here a self consistent many-bodyapproach reveals the close interlink of the properties of D meson andopen-charm baryon resonances in nuclear matter. The relevance of exotic baryonresonances for the spectral distortion of the $D_s^\\pm$ in nuclear matter ispointed out.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present metallicities and their variations with different parameters for36 high-latitude fields covering Galactic longitudes 0<l<360. The metallicitiesfor relatively short vertical distances (z<2.5 kpc) show systematicfluctuations with Galactic longitude, similar to those of the thick-discscaleheight, which may be interpreted as indicating a common origin, viz., theflare effect of the disc. This suggestion is supported by the metallicityvariations which we find as functions of radial distance. The metallicityvariation at larger vertical distances (6.5<z<9.5 kpc) is small but monotonic.Three different vertical metallicity gradients could be detected:d[M/H]/dz=-0.22(+/-0.03), d[M/H]/dz=-0.38 (+/-0.06), and d[M/H]/dz=-0.08(+/-0.07) dex/kpc for the intervals z<3, 3<z<5, and 5<z<10 kpc, respectively.Since our data cover the whole Galactic longitude interval, the resultingmetallicity gradients can be interpreted as properties of the larger-scaleGalaxy. The first gradient confirms the dissipational formation of the disc atshort z-distances. The steeper gradient corresponds to the transition regionbetween different population components of the Galaxy, and finally, the lowestvalue provides an adequate description of the inner-halo metallicity gradient.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The high volume of packets and packet rates of traffic on some router linksmakes it exceedingly difficult for routers to examine every packet in order tokeep detailed statistics about the traffic which is traversing the router.Sampling is commonly applied on routers in order to limit the load incurred bythe collection of information that the router has to undertake when evaluatingflow information for monitoring purposes. The sampling process in nearly allcases is a deterministic process of choosing 1 in every N packets on aper-interface basis, and then forming the flow statistics based on thecollected sampled statistics. Even though this sampling may not be significantfor some statistics, such as packet rate, others can be severely distorted.However, it is important to consider the sampling techniques and their relativeaccuracy when applied to different traffic patterns. The main disadvantage ofsampling is the loss of accuracy in the collected trace when compared to theoriginal traffic stream. To date there has not been a detailed analysis of theimpact of sampling at a router in various traffic profiles and flow criteria.In this paper, we assess the performance of the sampling process as used inNetFlow in detail, and we discuss some techniques for the compensation of lossof monitoring detail.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "In the context of Free Probability Theory, we study two differentconstructions that provide new examples of factors of type ${\\rm II_1}$ withprescribed fundamental group. First we investigate state-preserving groupactions on the almost periodic free Araki-Woods factors satisfying both acondition of mixing and a condition of free malleability in the sense of Popa.Typical examples are given by the free Bogoliubov shifts. Take an ICC $w$-rigidgroup $G$ such that $\\mathcal{F}(L(G)) = \\{1\\}$ (e.g. $G = \\Z^2 \\rtimes \\SL(2,\\Z)$). For any countable subgroup $S \\subset \\R^*_+$, we show that there existsan action of $G$ on $L(\\F_\\infty)$ such that $L(\\F_\\infty) \\rtimes G$ is a type${\\rm II_1}$ factor and its fundamental group is $S$. The second constructionis based on a free product. Take $(B(H), \\psi)$ any factor of type ${\\rm I}$endowed with a faithful normal state and denote by $\\Gamma \\subset \\R^*_+$ thesubgroup generated by the point spectrum of $\\psi$. We show that thecentralizer $(L(G) \\ast B(H))^{\\tau \\ast \\psi}$ is a type ${\\rm II_1}$ factorand its fundamental group is $\\Gamma$. Our proofs rely on Popa'sdeformation/rigidity strategy using his intertwining-by-bimodules technique.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We investigate the segregation of the extragalactic population via colourcriteria to produce an efficient and inexpensive methodology to select specificsource populations as a function of far-infrared flux. Combining galaxyevolution scenarios and a detailed spectral library of galaxies, we producesimulated catalogues incorporating segregation of the extragalactic populationinto component types (Normal, star-forming, AGN) via color cuts. As a practicalapplication we apply our criteria to the deepest survey to be undertaken in thefar-infrared with the AKARI (formerly ASTRO-F) satellite. Using thefar-infrared wavebands of the Far-Infrared Surveyor (FIS, one of thefocal-plane instruments on AKARI) we successfully segregate the normal,starburst and ULIRG populations. We also show that with additional MIR imagingfrom AKARI's Infrared Camera (IRC), significant contamination and/or degeneracycan be further decreased and show a particular example of the separation ofcool normal galaxies and cold ULIRG sources. We conclude that our criteriaprovide an efficient means of selecting source populations (including rareluminous objects) and produce colour-segregated source counts without therequirement of time intensive ground-based follow up to differentiate betweenthe general galaxy population.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Aims: We present a photometric study of the deeply eclipsing SW Sex-typenova-like cataclysmic variable star BH Lyn  Methods: Time-resolved V-band CCD photometry was obtained for seven nightsbetween 1999 and 2004.  Results: We determined 11 new eclipse timings of BH Lyn and derived a refinedorbital ephemeris with an orbital period of 0.155875577(14) day. During theobservations, BH Lyn was in high-state with V~15.5 mag. The star presents ~1.5mag deep eclipses with mean full-width at half-flux of 0.0683(+/-0.0054)P_orb.  The eclipse shape is highly variable, even changing form cycle to cycle. Thisis most likely due to accretion disc surface brightness distributionvariations, most probably caused by strong flickering. Time-dependent accretiondisc self-occultation or variations of the hot spot(s) intensity are alsopossible explanations. Negative superhumps with period of ~0.145 day aredetected in two long runs in 2000. A possible connection between SW Sex andnegative superhump phenomena through the presence of tilted accretion disc isdiscussed, and a way to observationally test this is suggested.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The past three decades of investigation on nuclear physics and pulsarastrophysics have seen gradual recognition that elastodynamic approach to thecontinuum mechanics of nuclear matter provides proper account of macroscopicmotions of degenerate Fermi-matter constituting interior of the nuclearmaterial objects, the densest of all known today. This paper focuses on onetheoretical issue of this development which is concerned with oscillatorybehavior of a viscoelastic solid globe in the regime of quasistatic,force-free, non-compressional oscillations less investigated in the literaturecompared to oscillations in the regime of standing shear waves. We show that inthis case the problem of computing frequency and lifetime of spheroidal andtorsional modes of non-radial shear vibrations damped by viscosity can beunambiguously resolved by working from the energy balance equation and takingadvantage of the Rayleigh's variational method. The efficiency of this methodis demonstrated by solid globe models of nuclear physics and pulsarastrophysics dealing with oscillations of a spherical mass of a viscoelasticFermi-solid with homogeneous and non-homogeneous profiles of the bulk density,the shear modulus, and the shear viscosity.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We show that the surface gravity of a transiting extrasolar planet can becalculated from only the spectroscopic orbit of its parent star and theanalysis of its transit light curve. This does not require additionalconstraints, such as are often inferred from theoretical stellar models ormodel atmospheres. The planet's surface gravity can therefore be measuredprecisely and from only directly observable quantities. We outline the methodand apply it to the case of the first known transiting extrasolar planet, HD209458b. We find a surface gravity of g_p = 9.28 +/- 0.15 m/s, which is anorder of magnitude more precise than the best available measurements of itsmass, radius and density. This confirms that the planet has a much lowersurface gravity that that predicted by published theoretical models of gasgiant planets. We apply our method to all fourteen known transiting extrasolarplanets and find a significant correlation between surface gravity and orbitalperiod, which is related to the known correlation between mass and period. Thiscorrelation may be the underlying effect as surface gravity is a fundamentalparameter in the evaporation of planetary atmospheres.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present new X-ray timing and spectral observations of PSR J1930+1852, theyoung energetic pulsar at the center of the non-thermal supernova remnantG54.1+0.3. Using data obtained with the Rossi X-ray Timing Explorer and ChandraX-ray observatories we have derived an updated timing ephemeris of the 136 mspulsar spanning 6 years. During this interval, however, the period evolutionshows significant variability from the best fit constant spin-down rate of$\\dot P = 7.5112(6) \\times 10^{-13}$ s s$^{-1}$, suggesting strong timing noiseand/or glitch activity. The X-ray emission is highly pulsed ($71\\pm5%$modulation) and is characterized by an asymmetric, broad profile ($\\sim 70%$duty cycle) which is nearly twice the radio width. The spectrum of the pulsedemission is well fitted with an absorbed power law of photon index $\\Gamma =1.2\\pm0.2$; this is marginally harder than that of the unpulsed component. Thetotal 2-10 keV flux of the pulsar is $1.7 \\times 10^{-12}$ erg cm$^{-2}$s$^{-1}$. These results confirm PSR J1930+1852 as a typical Crab-like pulsar.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The discovery of a flux excess in the far-ultraviolet (UV) spectrum ofelliptical galaxies was a major surprise in 1969. While it is now clear thatthis UV excess is caused by an old population of hot helium-burning starswithout large hydrogen-rich envelopes, rather than young stars, their originhas remained a mystery. Here we show that these stars most likely lost theirenvelopes because of binary interactions, similar to the hot subdwarfpopulation in our own Galaxy. We have developed an evolutionary populationsynthesis model for the far-UV excess of elliptical galaxies based on thebinary model developed by Han et al (2002, 2003) for the formation of hotsubdwarfs in our Galaxy. Despite its simplicity, it successfully reproducesmost of the properties of elliptical galaxies with a UV excess: the range ofobserved UV excesses, both in $(1550-V)$ and $(2000-V)$, and their evolutionwith redshift. We also present colour-colour diagrams for use as diagnostictools in the study of elliptical galaxies. The model has major implications forunderstanding the evolution of the UV excess and of elliptical galaxies ingeneral. In particular, it implies that the UV excess is not a sign of age, ashad been postulated previously, and predicts that it should not be stronglydependent on the metallicity of the population, but exists universally fromdwarf ellipticals to giant ellipticals.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "One of the major problems in computational biology is the inability ofexisting classification models to incorporate expanding and new domainknowledge. This problem of static classification models is addressed in thispaper by the introduction of incremental learning for problems inbioinformatics. Many machine learning tools have been applied to this problemusing static machine learning structures such as neural networks or supportvector machines that are unable to accommodate new information into theirexisting models. We utilize the fuzzy ARTMAP as an alternate machine learningsystem that has the ability of incrementally learning new data as it becomesavailable. The fuzzy ARTMAP is found to be comparable to many of the widespreadmachine learning systems. The use of an evolutionary strategy in the selectionand combination of individual classifiers into an ensemble system, coupled withthe incremental learning ability of the fuzzy ARTMAP is proven to be suitableas a pattern classifier. The algorithm presented is tested using data from theG-Coupled Protein Receptors Database and shows good accuracy of 83%. The systempresented is also generally applicable, and can be used in problems in genomicsand proteomics.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Simple nonlinear dynamical systems with multiple stable stationary states areoften taken as models for switchlike biological systems. This paper considersthe interaction of multiple such simple multistable systems when they areembedded together into a larger dynamical \"supersystem.\" Attention is focusedon the network structure of the resulting set of coupled differentialequations, and the consequences of this structure on the propensity of theembedded switches to act independently versus cooperatively. Specifically, itis argued that both larger average and larger variance of the node degreedistribution lead to increased switch independence. Given the frequency ofempirical observations of high variance degree distributions (e.g., power-law)in biological networks, it is suggested that the results presented here may aidin identifying switch-integrating subnetworks as comparatively homogenous,low-degree, substructures. Potential applications to ecological problems suchas the relationship of stability and complexity are also briefly discussed.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We analyze the effect of gravitational radiation reaction on generic orbitsaround a body with an axisymmetric mass quadrupole moment Q to linear order inQ, to the leading post-Newtonian order, and to linear order in the mass ratio.This system admits three constants of the motion in absence of radiationreaction: energy, angular momentum, and a third constant analogous to theCarter constant. We compute instantaneous and time-averaged rates of change ofthese three constants. For a point particle orbiting a black hole, Ryan hascomputed the leading order evolution of the orbit's Carter constant, which islinear in the spin. Our result, when combined with an interaction quadratic inthe spin (the coupling of the black hole's spin to its own radiation reactionfield), gives the next to leading order evolution. The effect of thequadrupole, like that of the linear spin term, is to circularize eccentricorbits and to drive the orbital plane towards antialignment with the symmetryaxis. In addition we consider a system of two point masses where one body has asingle mass multipole or current multipole. To linear order in the mass ratio,to linear order in the multipole, and to the leading post-Newtonian order, weshow that there does not exist an analog of the Carter constant for such asystem (except for the cases of spin and mass quadrupole). With mild additionalassumptions, this result falsifies the conjecture that all vacuum, axisymmetricspacetimes posess a third constant of geodesic motion.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Previous LHC forecasts for the constrained minimal supersymmetric standardmodel (CMSSM), based on current astrophysical and laboratory measurements, haveused priors that are flat in the parameter tan beta, while being constrained topostdict the central experimental value of MZ. We construct a different, newand more natural prior with a measure in mu and B (the more fundamental MSSMparameters from which tan beta and MZ are actually derived). We find that as aconsequence this choice leads to a well defined fine-tuning measure in theparameter space. We investigate the effect of such on global CMSSM fits toindirect constraints, providing posterior probability distributions for LargeHadron Collider (LHC) sparticle production cross sections. The change in priorshas a significant effect, strongly suppressing the pseudoscalar Higgs bosondark matter annihilation region, and diminishing the probable values ofsparticle masses. We also show how to interpret fit information from a MarkovChain Monte Carlo in a frequentist fashion; namely by using the profilelikelihood. Bayesian and frequentist interpretations of CMSSM fits are comparedand contrasted.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We study the possibility that the mutual interactions between Jupiter andSaturn prevented Type II migration from driving these planets much closer tothe Sun. Our work extends previous results by Masset and Snellgrove (2001), byexploring a wider set of initial conditions and disk parameters, and by using anew hydrodynamical code that properly describes for the global viscousevolution of the disk. Initially both planets migrate towards the Sun, andSaturn's migration tends to be faster. As a consequence, they eventually end uplocked in a mean motion resonance. If this happens in the 2:3 resonance, theresonant motion is particularly stable, and the gaps opened by the planets inthe disk may overlap. This causes a drastic change in the torque balance forthe two planets, which substantially slows down the planets' inward migration.If the gap overlap is substantial, planet migration may even be stopped orreversed. As the widths of the gaps depend on disk viscosity and scale height,this mechanism is particularly efficient in low viscosity, cool disks. Wediscuss the compatibility of our results with the initial conditions adopted inTsiganis et al. (2005) and Gomes et al. (2005) to explain the current orbitalarchitecture of the giant planets and the origin of the Late Heavy Bombardmentof the Moon.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The mechanism of carbon nanotube (CNT) nucleation and growth has been amystery for over 15 years. Prior models have attempted the extension of olderclassical transport mechanisms. In July 2000, a more detailed and accuratenonclassical, relativistic mechanism was formulated considering the detaileddynamics of the electronics of spin and orbital rehybridization between thecarbon and catalyst via novel mesoscopic phenomena and quantum dynamics.Ferromagnetic carbon was demonstrated. Here, quantum (Hall) effects andrelativistic effects of intense many body spin-orbital interactions for novelorbital rehybridization dynamics (Little Effect) are proposed in this newdynamical magnetic mechanism. This dynamic ferromagnetic mechanism is proven byimposing dynamic and static magnetic fields during CNT syntheses and observingthe different influence of these external magnetic environments on thecatalyzing spin currents and spin waves and the resulting CNT formation.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Dynamic magnetic susceptibility, $\\chi$, was studied in several intermetallicmaterials exhibiting ferromagnetic, antiferromagnetic and metamagnetictransitions. Precise measurements by using a 14 MHz tunnel diode oscillator(TDO) allow detailed insight into the field and temperature dependence of$\\chi$. In particular, local moment ferromagnets show a sharp peak in $\\chi(T)$near the Curie temperature, $T_c$. The peak amplitude decreases and shifts tohigher temperatures with very small applied dc fields. Anisotropic measurementsof CeVSb$_3$ show that this peak is present provided the magnetic easy axis isaligned with the excitation field. In a striking contrast, small moment,itinerant ferromagnets (i.e., ZrZn$_2$) show a broad maximum in $\\chi(T)$ thatresponds differently to applied field. We believe that TDO measurements providea very sensitive way to distinguish between local and itinerant moment magneticorders. Local moment antiferromagnets do not show a peak at the N\\'eeltemperature, $T_N$, but only a sharp decrease of $\\chi$ below $T_N$ due to theloss of spin-disorder scattering changing the penetration depth of the acexcitation field. Furthermore, we show that the TDO is capable of detectingchanges in spin order as well as metamagnetic transitions. Finally, criticalscaling of $\\chi(T,H)$ in the vicinity of $T_C$ is discussed in CeVSb$_3$ andCeAgSb$_2$.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present a rigorous calculation of the dynamical friction force exerted ona spherical massive perturber moving through an infinite homogenous system offield stars. By calculating the shape and mass of the polarization cloudinduced by the perturber in the background system, which decelerates the motionof the perturber, we recover Chandrasekhar's drag force law with a modifiedCoulomb logarithm. As concrete examples we calculate the drag force exerted ona Plummer sphere or a sphere with the density distribution of a Hernquistprofile. It is shown that the shape of the perturber affects only the exactform of the Coulomb logarithm. The latter converges on small scales, becauseencounters of the test and field stars with impact parameters less than thesize of the massive perturber become inefficient. We confirm this way earlierresults based on the impulse approximation of small angle scatterings.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "I argue that the (extended) Standard Model (SM) of particle physics and therenormalizable Feynman-Weinberg theory of quantum gravity comprise a theory ofeverything. I show that imposing the appropriate cosmological boundaryconditions make the theory finite. The infinities that are normallyrenormalized away and the series divergence infinities are both eliminated bythe same mechanism. Furthermore, this theory can resolve the horizon, flatness,and isotropy problems of cosmology. Joint mathematical consistency naturallyyields a scale-free, Gaussian, adiabatic perturbation spectrum, and more matterthan antimatter. I show that mathematical consistency of the theory requiresthe universe to begin at an initial singularity with a pure $SU(2)_L$ gaugefield. I show that quantum mechanics requires this field to have a Planckianspectrum whatever its temperature. If this field has managed to survivethermalization to the present day, then it would be the CMBR. If so, then wewould have a natural explanation for the dark matter and the dark energy. Ishow that isotropic ultrahigh energy (UHE) cosmic rays are explained if theCMBR is a pure $SU(2)_L$ gauge field. The $SU(2)_L$ nature of the CMBR may havebeen seen in the Sunyaev-Zel'dovich effect. I propose several simpleexperiments to test the hypothesis.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The LBV/WR system HD 5980 contains a short-period, eccentric binary systemwith interacting stellar winds. In this paper we summarize results from modelcalculations of the tidal flows on the LBV component showing that energydissipation rates, E-dot, associated with turbulent viscosity are orbital-phasedependent as well as variable over the stellar surface. We speculate that ifE-dot contributes towards driving mass-loss, the strongest wind-windinteraction effects may occur after periastron passage. In addition, the modelsuggests the presence of stronger outflows localized at polar angles theta~30--50 degrees during part of the orbital cycle. Thus, the analysis of wind-windinteractions in this system requires that models be revised to incorporatenon-stationary and asymmetric wind structures.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Using a large galaxy group catalogue based on the Sloan Digital Sky SurveyData Release 4 we measure three different types of intrinsic galaxy alignmentwithin groups: halo alignment between the orientation of the brightest groupgalaxies (BGG) and the distribution of its satellite galaxies, radial alignmentbetween the orientation of a satellite galaxy and the direction towards itsBGG, and direct alignment between the orientation of the BGG and that of itssatellites. In agreement with previous studies we find that satellite galaxiesare preferentially located along the major axis. In addition, on scales r < 0.7Rvir we find that red satellites are preferentially aligned radially with thedirection to the BGG. The orientations of blue satellites, however, areperfectly consistent with being isotropic. Finally, on scales r < 0.1 \\Rvir, wefind a weak but significant indication for direct alignment between satellitesand BGGs. We briefly discuss the implications for weak lensing measurements.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "In this paper, we first discuss the general properties of anintermediate-statistics quantum bracket, $[ u,v]_{n}=uv-e^{i2\\pi /(n+1)}vu$,which corresponds to intermediate statistics in which the maximum occupationnumber of one quantum state is an arbitrary integer, $n$. A further study ofthe operator realization of intermediate statistics is given. We construct theintermediate-statistics coherent state. An intermediate-statistics oscillatoris constructed, which returns to bosonic and fermionic oscillators respectivelywhen $n\\to \\infty $ and $n=1$. The energy spectrum of such anintermediate-statistics oscillator is calculated. Finally, we discuss theintermediate-statistics representation of angular momentum ($su(2)$) algebra.Moreover, a further study of the operator realization of intermediatestatistics is given in the Appendix.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "A real-space quantum transport simulator for carbon nanoribbon (CNR) MOSFETshas been developed. Using this simulator, the performance of carbon nanoribbon(CNR) MOSFETs is examined in the ballistic limit. The impact of quantum effectson device performance of CNR MOSFETs is also studied. We found that 2Dsemi-infinite graphene contacts provide metal-induced-gap-states (MIGS) in theCNR channel. These states would provide quantum tunneling in the short channeldevice and cause Fermi level pining. These effects cause device performancedegradation both on the ON-state and the OFF-state. Pure 1D devices (infinitecontacts), however, show no MIGS. Quantum tunneling effects are still playingan important role in the device characteristics. Conduction due to band-to-bandtunneling is accurately captured in our simulations. It is important in thesedevices, and found to dominate the off-state current. Based on our simulations,both a 1.4nm wide and a 1.8nm wide CNR with channel length of 12.5nm canoutperform ultra scaled Si devices in terms of drive current capabilities andelectrostatic control. Although subthreshold slopes in the forward-biasconduction are better than in Si transistors, tunneling currents are importantand prevent the achievement of the theoretical limit of 60mV/dec.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We investigate the properties of the so-called BL Her stars, i.e., PopulationII Cepheids with periods shorter than 8 days, using updated pulsation modelsand evolutionary tracks computed adopting a metal abundance in the range ofZ=0.0001 to Z=0.004. We derive the predicted Period-Magnitude (PM) andPeriod-Wesenheit (PW) relations at the various photometric bands and we showthat the slopes of these relations are in good agreement with the slopesdetermined by observed variables in Galactic globular clusters, independentlyof the adopted M_V(RR)-[Fe/H] relation to get the cluster RR Lyrae-baseddistance. Moreover, we show that also the distances provided by the predictedPM and PW relations for BL Her stars agree within the errors with the RR Lyraebased values. The use of the predicted relations with W Vir stars, which arePopulation II Cepheids with periods longer than 8 days, provides no clearevidence for or against a change in the PM and PW slopes around P~10 days.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Long, cylindrical metal nanowires have recently been observed to form and bestable for seconds at a time at room temperature. Their stability andstructural dynamics is well described by a continuum model, the nanoscalefree-electron model, which predicts cylinders in certain intervals of radius tobe linearly unstable. In this paper, I study how a small, localizedperturbation of such an unstable wire grows exponentially and propagates alongthe wire with a well-defined front. The front is found to be pulled, and formsa coherent pattern behind it. It is well described by a linear marginalstability analysis of front propagation into an unstable state. In some cases,nonlinearities of the wire dynamics are found to trigger an invasive mode thatpushes the front. Experimental procedures that could lead to the observation ofthis phenomenon are suggested.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "In contrast to the Euler-Poincar{\\'e} reduction of geodesic flows of left- orright-invariant metrics on Lie groups to the corresponding Lie algebra (or itsdual), one can consider the reduction of the geodesic flows to the groupitself. The reduced vector field has a remarkable hydrodynamic interpretation:it is a velocity field for a stationary flow of an ideal fluid. Right- orleft-invariant symmetry fields of the reduced field define vortex manifolds forsuch flows.  Consider now a mechanical system, whose configuration space is a Lie groupand whose Lagrangian is invariant to left translations on that group, andassume that the mass geometry of the system may change under the action ofinternal control forces. Such system can also be reduced to the Lie group. Withno controls, this mechanical system describes a geodesic flow of theleft-invariant metric, given by the Lagrangian, and thus its reduced flow is astationary ideal fluid flow on the Lie group. The standard control problem forsuch system is to find the conditions, under which the system can be broughtfrom any initial position in the configuration space to another preassignedposition by changing its mass geometry. We show that under these conditions, bychanging the mass geometry, one can also bring one vortex manifold to any otherpreassigned vortex manifold.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "For the 100 largest European universities we studied the statisticalproperties of bibliometric indicators related to research performance, fieldcitation density and journal impact. We find a size-dependent cumulativeadvantage for the impact of universities in terms of total number of citations.In previous work a similar scaling rule was found at the level of researchgroups. Therefore we conjecture that this scaling rule is a prevalent propertyof the science system. We observe that lower performance universities have alarger size-dependent cumulative advantage for receiving citations thantop-performance universities. We also find that for the lower-performanceuniversities the fraction of not-cited publications decreases considerably withsize. Generally, the higher the average journal impact of the publications of auniversity, the lower the number of not-cited publications. We find that theaverage research performance does not dilute with size. Large top-performanceuniversities succeed in keeping a high performance over a broad range ofactivities. This most probably is an indication of their scientific attractivepower. Next we find that particularly for the lower-performance universitiesthe field citation density provides a strong cumulative advantage in citationsper publication. The relation between number of citations and field citationdensity found in this study can be considered as a second basic scaling rule ofthe science system. Top-performance universities publish in journals withsignificantly higher journal impact as compared to the lower performanceuniversities. We find a significant decrease of the fraction of self-citationswith increasing research performance, average field citation density, andaverage journal impact.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We compare waveforms obtained by numerically evolving nonspinning binaryblack holes to post-Newtonian (PN) template families currently used in thesearch for gravitational waves by ground-based detectors. We find that thetime-domain 3.5PN template family, which includes the inspiral phase, hasfitting factors (FFs) >= 0.96 for binary systems with total mass M = 10 ~ 20Msun. The time-domain 3.5PN effective-one-body template family, which includesthe inspiral, merger and ring-down phases, gives satisfactory signal-matchingperformance with FFs >= 0.96 for binary systems with total mass M = 10 ~ 120Msun. If we introduce a cutoff frequency properly adjusted to the finalblack-hole ring-down frequency, we find that the frequency-domainstationary-phase-approximated template family at 3.5PN order has FFs >= 0.96for binary systems with total mass M = 10 ~ 20 Msun. However, to obtain highmatching performances for larger binary masses, we need to either extend thisfamily to unphysical regions of the parameter space or introduce a 4PN ordercoefficient in the frequency-domain GW phase. Finally, we find that thephenomenological Buonanno-Chen-Vallisneri family has FFs >= 0.97 with totalmass M=10 ~ 120Msun. The main analyses use the noise spectral-density of LIGO,but several tests are extended to VIRGO and advanced LIGO noise-spectraldensities.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "A scale invariant model containing dilaton $\\phi$ and dust (as a model ofmatter) is studied where the shift symmetry $\\phi\\to\\phi +const.$ isspontaneously broken at the classical level due to intrinsic features of themodel. The dilaton to matter coupling \"constant\" $f$ appears to be dependent ofthe matter density. In normal conditions, i.e. when the matter energy densityis many orders of magnitude larger than the dilaton contribution to the darkenergy density, $f$ becomes less than the ratio of the \"mass of the vacuum\" inthe volume occupied by the matter to the Planck mass. The model yields thiskind of \"Archimedes law\" without any especial (intended for this) choice of theunderlying action and without fine tuning of the parameters. The model not onlyexplains why all attempts to discover a scalar force correction to Newtoniangravity were unsuccessful so far but also predicts that in the near futurethere is no chance to detect such corrections in the astronomical measurementsas well as in the specially designed fifth force experiments on intermediate,short (like millimeter) and even ultrashort (a few nanometer) ranges. Thisprediction is alternative to predictions of other known models.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We revisit the problem of interplay between the strong and the Coulombinteraction in the charged-to-neutral yield ratio for $B {\\bar B}$ and $D {\\barD}$ pairs near their respective thresholds in $e^+e^-$ annihilation. Weconsider here a realistic situation with a resonant interaction in the isospinI=0 channel and a nonresonant strong scattering amplitude in the I=1 state. Wefind that the yield ratio has a smooth behavior depending on the scatteringphase in the I=1 channel. The same approach is also applicable to the $K {\\barK}$ production at the $\\phi(1020)$ resonance, where the Coulomb effect in thecharged-to-neutral yield ratio is generally sensitive to the scattering phasesin both the isoscalar and the isovector channels. Furthermore, we apply thesame approach to the treatment of the effect of the isotopic mass differencebetween the charged and neutral mesons and argue that the strong-scatteringeffects generally result in a modification to the pure kinematical effect ofthis mass difference.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We discuss two models for describing the behavior of matter at largedensities and intermediate temperatures. In both models a softening of theequation of state takes place due to the appearance of new degrees of freedom.The first is a hadronic model in which the softening is due to chiral symmetryrestoration. In the second model the softening is associated with the formationof clusters of quarks in the mixed phase. We show that both models allow asignificant softening but, in the first case the bulk modulus is mainlydependent on the density, while in the mixed phase model it also stronglydepends on the temperature. We also show that the bulk modulus is not vanishingin the mixed phase due to the presence of two conserved charges, the baryon andthe isospin one. Only in a small region of densities and temperatures theincompressibility becomes extremely small. Finally we compare our results withrecent analysis of heavy ion collisions at intermediate energies.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present results of an attempt to include more detailed gas physicsmotivated from hydrodynamical simulations within semi-analytic models (SAM) ofgalaxy formation, focusing on the role that environmental effects play. Themain difference to previous SAMs is that we include 'gravitational' heating ofthe intra-cluster medium (ICM) by the net surplus of gravitational potentialenergy released from gas that has been stripped from infalling satellites.Gravitational heating appears to be an efficient heating source able to preventcooling in environments corresponding to dark matter halos more massive than$\\sim 10^{13} $M$_{\\odot}$. The energy release by gravitational heating canmatch that by AGN-feedback in massive galaxies and can exceed it in the mostmassive ones. However, there is a fundamental difference in the way the twoprocesses operate. Gravitational heating becomes important at late times, whenthe peak activity of AGNs is already over, and it is very mass dependent. Thismass dependency and time behaviour gives the right trend to recover down-sizingin the star-formation rate of massive galaxies. Abridged...", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present optical and near-infrared light curves of SN 2001el from 310 to445 days past maximum light, obtained with the Very Large Telescope. Thelate-time optical (UBVRI) light curves decay in a nearly linear fashion withdecay time scales of 1.43\\pm0.14, 1.43\\pm0.06, 1.48\\pm0.06, 1.45\\pm0.07, and1.03\\pm0.07 magnitudes (per hundred days) in the U, B, V, R and I bands,respectively. In contrast, in the near-infrared (JHKs) bands the time evolutionof the flux appears to be nearly constant at these epochs. We measure declinerates (per hundred days) of 0.19\\pm0.10 and 0.17\\pm0.11 magnitudes in the J andH bands, respectively. We construct a UVOIR light curve, and find that thelate-time luminosity has a decay time scale nearly consistent with completedepostion of positron kinetic energy. The late-time light curves of the normaltype Ia SN 2001el demonstrate the increased importance of the near-infraredcontribution. This was previously observed in the peculiar SN 2000cx, and theresults for SN 2001el thus ensure that the conclusions previously based on asingle peculiar event are applicable to normal type Ia supernovae. The measuredlate-time UVOIR decline rate suggests that a majority of the positrons aretrapped within the ejecta. This results does not favor the predictions of aweak and/or radially combed magnetic field configuration.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The IEEE 802.11e standard revises the Medium Access Control (MAC) layer ofthe former IEEE 802.11 standard for Quality-of-Service (QoS) provision in theWireless Local Area Networks (WLANs). The Enhanced Distributed Channel Access(EDCA) function of 802.11e defines multiple Access Categories (AC) withAC-specific Contention Window (CW) sizes, Arbitration Interframe Space (AIFS)values, and Transmit Opportunity (TXOP) limits to support MAC-level QoS andprioritization. We propose an analytical model for the EDCA function whichincorporates an accurate CW, AIFS, and TXOP differentiation at any trafficload. The proposed model is also shown to capture the effect of MAC layerbuffer size on the performance. Analytical and simulation results are comparedto demonstrate the accuracy of the proposed approach for varying traffic loads,EDCA parameters, and MAC layer buffer space.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The large-scale organization of the world economies is exhibitingincreasingly levels of local heterogeneity and global interdependency.Understanding the relation between local and global features calls foranalytical tools able to uncover the global emerging organization of theinternational trade network. Here we analyze the world network of bilateraltrade imbalances and characterize its overall flux organization, unravelinglocal and global high-flux pathways that define the backbone of the tradesystem. We develop a general procedure capable to progressively filter out in aconsistent and quantitative way the dominant trade channels. This procedure iscompletely general and can be applied to any weighted network to detect theunderlying structure of transport flows. The trade fluxes properties of theworld trade web determines a ranking of trade partnerships that highlightsglobal interdependencies, providing information not accessible by simple localanalysis. The present work provides new quantitative tools for a dynamicalapproach to the propagation of economic crises.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We quantify the effect of supernova Type Ia peculiar velocities on thederivation of cosmological parameters. The published distant and local Ia SNeused for the Supernova Legacy Survey first-year cosmology report form thesample for this study. While previous work has assumed that the local SNe areat rest in the CMB frame (the No Flow assumption), we test this assumption byapplying peculiar velocity corrections to the local SNe using three differentflow models. The models are based on the IRAS PSCz galaxy redshift survey, havevarying beta = Omega_m^0.6/b, and reproduce the Local Group motion in the CMBframe. These datasets are then fit for w, Omega_m, and Omega_Lambda usingflatness or LambdaCDM and a BAO prior. The chi^2 statistic is used to examinethe effect of the velocity corrections on the quality of the fits. The mostfavored model is the beta=0.5 model, which produces a fit significantly betterthan the No Flow assumption, consistent with previous peculiar velocitystudies. By comparing the No Flow assumption with the favored models we derivethe largest potential systematic error in w caused by ignoring peculiarvelocities to be Delta w = +0.04. For Omega_Lambda, the potential error isDelta Omega_Lambda = -0.04 and for Omega_m, the potential error is DeltaOmega_m < +0.01. The favored flow model (beta=0.5) produces the followingcosmological parameters: w = -1.08 (+0.09,-0.08), Omega_m = 0.27 (+0.02,-0.02)assuming a flat cosmology, and Omega_Lambda = 0.80 (+0.08,-0.07) and Omega_m =0.27 (+0.02,-0.02) for a w = -1 (LambdaCDM) cosmology.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The symmetric heavy-light ansatz is a method for finding the ground state ofany dilute unpolarized system of attractive two-component fermions.Operationally it can be viewed as a generalization of the Kohn-Sham equationsin density functional theory applied to N-body density correlations. While theoriginal Hamiltonian has an exact Z_2 symmetry, the heavy-light ansatz breaksthis symmetry by skewing the mass ratio of the two components. In the limitwhere one component is infinitely heavy, the many-body problem can be solved interms of single-particle orbitals. The original Z_2 symmetry is recovered byenforcing Z_2 symmetry as a constraint on N-body density correlations for thetwo components. For the 1D, 2D, and 3D attractive Hubbard models the method isin very good agreement with exact Lanczos calculations for few-body systems atarbitrary coupling. For the 3D attractive Hubbard model there is very goodagreement with lattice Monte Carlo results for many-body systems in the limitof infinite scattering length.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We investigated the viability of neutralino dark matter in the gaugemediation from emergent supersymmetry proposal. In this proposal, supersymmetryis broken at Planck scale and consequently, the gravitino is superheavy andcompletely decouples from the low energy theory. Squarks and sleptons obtaintheir soft masses dominantly through gauge mediation with other mechanismshighly suppressed. The lightest supersymmetric partner, in contrast totraditional gauge mediation, is a neutralino which is also a dark mattercandidate. By explicit calculation of the low energy spectra, the parameterspace was constrained using the WMAP observed relic density of dark matter,LEP2 Higgs mass bounds, collider bounds on supersymmetric partners and exoticB-meson decays. We found that the model has intriguing hybrid features such asa nearly gauge-mediated spectrum (the exception being the superheavy gravitino)but with a dominant mSUGRA-like bino-stau coannihilation channel and at large$\\tan \\beta$, A-resonance-like annihilation.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We investigate the behaviour of an original traffic model. The modelconsiders a single multi-lane street, populated by autonomous vehicles directedfrom either end to the other. Lanes have no intrinsic directionality, and thevehicles are inserted at random at either end and any lane. Collision avoidanceis fully automatic and, to enhance the transport capacity of the street,vehicles form_trains_ in which they may travel at high speed quite close to thevehicle in front.  We report on the transit times for vehicles under a wide variety ofconditions: vehicle insertion probability & imbalance and their maximum speeddistribution. We also outline an interesting feature of the model, that thecomplex interactions of many vehicles are considerably more powerful than asimple \"keep left\" directive which each vehicle should obey.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Topological excitations are believed to play an important role in differentareas of physics. For example, one case of topical interest is the use of dualmodels of quantum cromodynamics to understand properties of its vacuum andconfinement through the condensation of magnetic monopoles and vortices. Otherapplications are related to the role of these topological excitations,nonhomogeneous solutions of the field equations, in phase transitionsassociated to spontaneous symmetry breaking in gauge theories, whose study isof importance in phase transitions in the early universe, for instance. Here weshow a derivation of a model dual to the scalar Abelian Higgs model where itstopological excitations, namely vortex-strings, become manifest and can betreated in a quantum field theory way. The derivation of the nontrivialcontribution of these vacuum excitations to phase transitions and its analogywith superconductivity is then made possible and they are studied here.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The Debye-H\\\"uckel theory describes rigorously the thermal equilibrium ofclassical Coulomb fluids in the high-temperature $\\beta\\to 0$ regime ($\\beta$denotes the inverse temperature). It is generally believed that theDebye-H\\\"uckel theory and the systematic high-temperature expansion provide anadequate description also in the region of small {\\em strictly positive} valuesof $\\beta>0$. This hypothesis is tested in the present paper on atwo-dimensional Coulomb gas of pointlike $+/-$ unit charges interacting via alogarithmic potential which is equivalent to an integrable sine-Gordon fieldmodel. In particular, we apply a form factor method to obtain the exactasymptotic large-distance behavior of particle correlation functions,considered in the charge and number density combinations. We first determinethe general forms of the leading and subleading asymptotic terms at strictlypositive $\\beta>0$ and then evaluate their high-temperature $\\beta\\to 0$ forms.In the case of the {\\em charge} correlation function, the leading asymptoticterm at a strictly positive $\\beta>0$ is also the leading one in thehigh-temperature $\\beta\\to 0$ regime. On the contrary, the $\\beta\\to 0$behavior of the {\\em number density} correlation function is accompanied by aninterference between the first two asymptotic terms. Consequently, thelarge-distance behavior of this function exhibits a discontinuity when goingfrom strictly positive values of $\\beta>0$ to the Debye-H\\\"uckel limit$\\beta\\to 0$. This is the crucial conclusion of the paper: the large-distanceasymptotics and the high-temperature limit do not commute for the densitycorrelation function of the two-dimensional Coulomb gas.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Data from {\\it Chandra} observations of thirty nearby galaxies were analyzedand 365 X-ray point sources were chosen whose spectra were not contaminated byexcessive diffuse emission and not affected by photon pile up. The spectra ofthese sources were fitted using two spectral models (an absorbed power-law anda disk blackbody) to ascertain the dependence of estimated parameters on thespectral model used. It was found that the cumulative luminosity functiondepends on the choice of the spectral model, especially for luminosities $>10^{40}$ ergs/s. In accordance with previous results, a large number ($\\sim80$) of the sources have luminosities $> 10^{39}$ ergs/s (Ultra-Luminous X-raysources) with indistinguishable average spectral parameters (inner disktemperature $\\sim 1$ keV and/or photon index $\\Gamma \\sim 2$) with those of thelower luminosities ones. After considering foreground stars and knownbackground AGN,we identify four sources whose minimum luminosity exceed$10^{40}$ ergs/s, and call them Extremely Luminous X-ray sources (ELX). Thespectra of these sources are in general better represented by the disk blackbody model than the power-law one. These ELX can be grouped into two distinctspectral classes. Two of them have an inner disk temperature of $< 0.5$ keV andhence are called ``supersoft'' ELX, while the other two have temperatures$\\gtrsim 1.3$ keV and are called ``hard'' ELX. The estimated inner disktemperatures of the supersoft ELX are compatible with the hypothesis that theyharbor intermediate size black holes, which are accreting at $\\sim 0.5$ timestheir Eddington Luminosity. The radiative mechanism for hard ELX, seems to beInverse Comptonization, which in contrast to standard black holes systems, isprobably saturated.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Rigorous computer simulations of propagating electromagnetic fields havebecome an important tool for optical metrology and optics design ofnanostructured components. As has been shown in previous benchmarks some of thepresently used methods suffer from low convergence rates and/or low accuracy ofthe results and exhibit very long computation times which makes application toextended 2D layout patterns impractical. We address 3D simulation tasks byusing a finite-element solver which has been shown to be superior to competingmethods by several orders of magnitude in accuracy and computational time fortypical microlithography simulations. We report on the current status of thesolver, incorporating higher order edge elements, adaptive refinement methods,and fast solution algorithms. Further, we investigate the performance of thesolver in the 3D simulation project of light diffraction off an alternatingphase-shift contact-hole mask.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Quantum gravity is analyzed from the viewpoint of the renormalization group.The analysis is based on methods introduced by J. Polchinski concerning theperturbative renormalization with flow equations. In the first part of thiswork, the program of renormalization with flow equations is reviewed and thenextended to effective field theories that have a finite UV cutoff. This is donefor a scalar field theory by imposing additional renormalization conditions forsome of the nonrenormalizable couplings. It turns out that one so obtains astatement on the predictivity of the effective theory at scales far below theUV cutoff. In particular, nonrenormalizable theories can be treated withoutproblems in the proposed framework. In the second part, the standard covariantBRS quantization program for Euclidean Einstein gravity is applied. A momentumcutoff regularization is imposed and the resulting violation of theSlavnov-Taylor identities is discussed. Deriving Polchinski's renormalizationgroup equation for Euclidean quantum gravity, the predictivity of effectivequantum gravity at scales far below the Planck scale is investigated with flowequations. A fine-tuning procedure for restoring the violated Slavnov-Tayloridentities is proposed and it is argued that in the effective quantum gravitycontext, the restoration will only be accomplished with finite accuracy.Finally, the no-cutoff limit of Euclidean quantum gravity is analyzed from theviewpoint of the Polchinski method. It is speculated whether a limit withnonvanishing gravitational constant might exist where the latter wouldultimatively be determined by the cosmological constant and the masses of theelementary particles.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "In many applications it will be useful to know those patterns that occur witha balanced interval, e.g., a certain combination of phone numbers are calledalmost every Friday or a group of products are sold a lot on Tuesday andThursday.  In previous work we proposed a new measure of support (the number ofoccurrences of a pattern in a dataset), where we count the number of times apattern occurs (nearly) in the middle between two other occurrences. If thenumber of non-occurrences between two occurrences of a pattern stays almost thesame then we call the pattern balanced.  It was noticed that some very frequent patterns obviously also occur with abalanced interval, meaning in every transaction. However more interestingpatterns might occur, e.g., every three transactions. Here we discuss asolution using standard deviation and average. Furthermore we propose a simplerapproach for pruning patterns with a balanced interval, making estimating thepruning threshold more intuitive.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "This thesis consists of two parts which share only a slight overlap.  The first part is concerned with the study of ideals in the ring$C^\\infty(M,R)$ of smooth functions on a compact smooth manifold M or moregenerally submodules of a finitely generated $C^\\infty(M,R)$-module V. Wedefine a topology on the space of all submodules of V of a fixed finitecodimension d. Its main property is that it is compact Hausdorff and, in thecase of ideals in the ring itself, it contains as a subspace the configurationspace of d distinct unordered points in M and therefore gives a\"compactification\" of this configuration space. We present a concretedescription of this space for low codimensions.  The main focus is then put on the second part which is concerned with ageneralization of Vassiliev's h-principle. This principle in its simplest formasserts that the jet prolongation map $j^r:C^\\infty(M,E)\\to\\Gamma(J^r(M,E))$,defined on the space of smooth maps from a compact manifold M to a Euclideanspace E and with target the space of smooth sections of the jet bundle$J^r(M,E)$, is a cohomology isomorphism when restricted to certain\"nonsingular\" subsets (these are defined in terms of a certain subset$R\\subseteq J^r(M,E)$). Our generalization then puts this theorem in a moregeneral setting of topological $C^\\infty(M,R)$-modules. As a reward we get astrengthening of this result asserting that all the homotopy fibres have zerohomology.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Many systems of different nature exhibit scale free behaviors. Economicsystems with power law distribution in the wealth is one of the examples. Tobetter understand the working behind the complexity, we undertook an empiricalstudy measuring the interactions between market participants. A Web server wassetup to administer the exchange of futures contracts whose liquidation priceswere coupled to event outcomes. After free registration, participants startedtrading to compete for the money prizes upon maturity of the futures contractsat the end of the experiment. The evolving `cash' flow network wasreconstructed from the transactions between players. We show that the networktopology is hierarchical, disassortative and scale-free with a power lawexponent of 1.02+-0.09 in the degree distribution. The small-world propertyemerged early in the experiment while the number of participants was stillsmall. We also show power law distributions of the net incomes andinter-transaction time intervals. Big winners and losers are associated withhigh degree, high betweenness centrality, low clustering coefficient and lowdegree-correlation. We identify communities in the network as groups of thelike-minded. The distribution of the community sizes is shown to be power-lawdistributed with an exponent of 1.19+-0.16.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present millimeter and radio observations of 13 SDSS quasars at reshiftsz~6. We observed eleven of them with the Max-Planck Millimeter Bolometer Array(MAMBO-2) at the IRAM 30m-telescope at 250 GHz and all of them with the VeryLarge Array (VLA) at 1.4 GHz. Four sources are detected by MAMBO-2 and six aredetected by the VLA at >=3 sigma level. These sources, together with another 6published in previous papers,yield a submillimeter/millimeter and radioobserved SDSS quasar sample at z~6. We use this sample to investigate thefar-infrared (FIR) andradio properties of optically bright quasars in the earlyuniverse. We compare this sample to lower redshift samples of quasars observedinthe submillimeter and millimeter wavelengths ((sub)mm), and find that thedistribution of the FIR to B band optical luminosity ratio (L_FIR/L_B) issimilar from z~2 to 6. We find a weak correlation between the FIR luminosity(L_FIR) and B band optical luminosity (L_B) byincluding the (sub)mm observedsamples at all redshifts. Some strong (sub)mm detections in the z~6 sample haveradio-to-FIR ratios within the range defined by star forming galaxies, whichsuggests possible co-eval star forming activity with the powerful AGN in thesesources. We calculate the rest frame radio to optical ratios (R*_1.4=L_{v,1.4GHz}/L_{v, 4400A}) for all of the VLA observed sources in the z~6 quasarsample. Only one radio detection in this sample, J083643.85+005453.3, hasR*_1.4~40 and can be considered radio loud. There are no strong radio sources(R*_1.4>=100) among these SDSS quasars at z~6. These data are consistent with,although do not set strong constraints on, a decreasing radio-loud quasarfraction with increasing redshift.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We investigate the evolution of binary fractions in star clusters usingN-body models of up to 100000 stars. Primordial binary frequencies in thesemodels range from 5% to 50%. Simulations are performed with the NBODY4 code andinclude a full mass spectrum of stars, stellar evolution, binary evolution andthe tidal field of the Galaxy. We find that the overall binary fraction of acluster almost always remains close to the primordial value, except at latetimes when a cluster is near dissolution. A critical exception occurs in thecentral regions where we observe a marked increase in binary fraction with time-- a simulation starting with 100000 stars and 5% binaries reached a corebinary frequency as high as 40% at the end of the core-collapse phase(occurring at 16 Gyr with ~20000 stars remaining). Binaries are destroyed inthe core by a variety of processes as a cluster evolves, but the combination ofmass-segregation and creation of new binaries in exchange interactions producesthe observed increase in relative number. We also find that binaries are cycledinto and out of cluster cores in a manner that is analogous to convection instars. For models of 100000 stars we show that the evolution of the core-radiusup to the end of the initial phase of core-collapse is not affected by theexact value of the primordial binary frequency (for frequencies of 10% orless). We discuss the ramifications of our results for the likely primordialbinary content of globular clusters.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present 6.5-meter MMT spectrophotometry of 20 H II regions in 13 extremelymetal-poor emission-line galaxies selected from the Data Release 5 of the SloanDigital Sky Survey to have [O III] 4959/Hbeta < 1 and [N II] 6583/Hbeta < 0.05.The electron temperature-sensitive emission line [O III] 4363 is detected in 13H II regions allowing a direct abundance determination. The oxygen abundance inthe remaining H II regions is derived using a semi-empirical method. The oxygenabundance of the galaxies in our sample ranges from 12+logO/H ~ 7.1 to ~ 7.8,with 10 H II regions having an oxygen abundance lower than 7.5. The lowestoxygen abundances, 12+logO/H = 7.14+/-0.03 and 7.13+/-0.07, are found in two HII regions of the blue compact dwarf galaxy SDSSJ0956+2849=DDO 68, making itthe second most-metal deficient emission-line galaxy known, after SBS0335-052W.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We address the problem of the factors contributing to a peak color trend ofold metal-rich globular cluster (MRGC) populations with mass of their hosts,early-type galaxies and spheroidal subsystems of spiral ones (spheroids). Thecolor-mass trend is often converted to a metallicity-mass trend under theassumption that age effects are small or negligible. While direct estimates ofthe ages of MRGC populations neither can rule out nor reliably support thepopulations' age trend, key data on timing of the formation of spheroids andother indirect evidence imply it in the sense: the more massive spheroid theolder on average its MRGC population. We show that the contribution of anallowable age trend of the MRGC populations to their peak color trend canachieve up to ~50 % or so. In this event the comparable value of the colortrend, ~30 %, is due to alpha-element ratio systematic variations of the orderof Delta[alpha/Fe] ~ 0.1 to 0.2 dex because of a correlation between the[alpha/Fe] ratios and age. Hence a systematic variation of exactly [Fe/H]ratios may turn out to be less significant among the contributors, and itsrange many times lower, i.e. of the order of Delta[Fe/H] ~ 0.1 or even none,than the corresponding range deduced by assuming no age trend.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "At the quantization of fields, due to the non-linear character of the timereversal, the creation-annihilation operators for the negative frequency modesshould be replaced to the operators of antiparticles not directly in the fieldoperators, but in the operator products. For the standard minimal Lagrangians(asymmetrical under the complex conjugated fields) it is shown that the chargeconjugation (C-) symmetry conditions for the Hamiltonian and the chargeoperator lead to the identities for the operator products allowing one toreplace the negative frequency operator products to the positive frequencyones. At the same time the operators in observables become normal ordered andthe zero-point energy does not appear. Only the symmetrized under the fieldoperators Lagrangians lead to the zero-point energy. The confrontation by theexperiments of the such C-symmetric quantization of fields and the solutionsome of the vacuum energy problems are discussed.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Magnetic fields likely play a key role in the dynamics and evolution ofprotoplanetary discs. They have the potential to efficiently transport angularmomentum by MHD turbulence or via the magnetocentrifugal acceleration ofoutflows from the disk surface, and magnetically-driven mixing has implicationsfor disk chemistry and evolution of the grain population. However, the weakionisation of protoplanetary discs means that magnetic fields may not be ableto effectively couple to the matter. I present calculations of the ionisationequilibrium and magnetic diffusivity as a function of height from the diskmidplane at radii of 1 and 5 AU. Dust grains tend to suppress magnetic couplingby soaking up electrons and ions from the gas phase and reducing theconductivity of the gas by many orders of magnitude. However, once grains havegrown to a few microns in size their effect starts to wane and magnetic fieldscan begin to couple to the gas even at the disk midplane. Because ions aregenerally decoupled from the magnetic field by neutral collisions whileelectrons are not, the Hall effect tends to dominate the diffusion of themagnetic field when it is able to partially couple to the gas.  For a standard population of 0.1 micron grains the active surface layers havea combined column of about 2 g/cm^2 at 1 AU; by the time grains have aggregatedto 3 microns the active surface density is 80 g/cm^2. In the absence of grains,x-rays maintain magnetic coupling to 10% of the disk material at 1 AU (150g/cm^2). At 5 AU the entire disk thickness becomes active once grains haveaggregated to 1 micron in size.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The numerical analysis of strongly interacting nanostructures requirespowerful techniques. Recently developed methods, such as the time-dependentdensity matrix renormalization group (tDMRG) approach or the embedded-clusterapproximation (ECA), rely on the numerical solution of clusters of finite size.For the interpretation of numerical results, it is therefore crucial tounderstand finite-size effects in detail. In this work, we present a carefulfinite-size analysis for the examples of one quantum dot, as well as threeserially connected quantum dots. Depending on odd-even effects, physicallyquite different results may emerge from clusters that do not differ much intheir size. We provide a solution to a recent controversy over results obtainedwith ECA for three quantum dots. In particular, using the optimum clustersdiscussed in this paper, the parameter range in which ECA can reliably beapplied is increased, as we show for the case of three quantum dots. As apractical procedure, we propose that a comparison of results for staticquantities against those of quasi-exact methods, such as the ground-statedensity matrix renormalization group (DMRG) method or exact diagonalization,serves to identify the optimum cluster type. In the examples studied here, wefind that to observe signatures of the Kondo effect in finite systems, the bestclusters involving dots and leads must have a total z-component of the spinequal to zero.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present measurements of the infrared response of the quasi-one-dimensionalorganic conductor (TMTSF)2$SO3 along (E||a) and perpendicular (E||b') to thestacking axis as a function of temperature. Above the metal-insulatortransition related to the anion ordering the optical conductivity spectra showa Drude-like response. Below the transition an energy gap of about 1500 cm-1(185 meV) opens, leading to the corresponding charge transfer band in theoptical conductivity spectra. The analysis of the infrared-active vibrationsgives evidence for the long-range crystal structure modulation below thetransition temperature and for the short-range order fluctuations of thelattice modulation above the transition temperature. Also we report about a newinfrared mode at around 710 cm-1 with a peculiar temperature behavior, whichhas so far not been observed in any other (TMTSF)2X salt showing ametal-insulator transition. A qualitative model based on the coupling betweenthe TMTSF molecule vibration and the reorientation of electrical dipole momentof the FSO3 anion is proposed, in order to explain the anomalous behavior ofthe new mode.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present new continuum VLA observations of the nearby Sy 1.5 galaxy NGC5033, made at 4.9 and 8.4 GHz on 8 April 2003. Combined with VLA archivalobservations at 1.4 and 4.9 GHz made on 7 August 1993, 29 August 1999, and 31October 1999, we sample the galaxy radio emission at scales ranging from thenuclear regions (<~ 100 pc) to the outer regions of the disk (~ 40 kpc). Thehigh-resolution VLA images show a core-jet structure for the Sy 1.5 nucleus.While the core has a moderately steep non-thermal radio spectrum (S_\\nu ~\\nu^\\alpha; \\alpha_{1.5}^{4.9} \\approx -0.4), the inner kpc region shows asteeper spectrum (\\alpha_{1.5}^{8.4} \\approx -0.9). This latter spectrum istypical of galaxies where energy losses are high, indicating that the escaperate of cosmic ray electrons in NGC 5033 is low. The nucleus contributes littleto the total 1.4 GHz radio power of NGC 5033 and, based on the radio tofar-infrared (FIR) relation, it appears that the radio and far-infraredemission from NGC 5033 are dominated by a starburst that during the last 10 Myrproduced stars at a rate of ~2.8 M_sun/yr, yielding a supernova (type Ib/c andII) rate of 0.045 #/yr. This supernova rate corresponds to about 1 SN eventevery 22 yr. Finally, from our deep 8.4 GHz VLA-D image, we suggest theexistence of a radio spur in NGC 5033, which could have been due to a hotsuperbubble formed as a consequence of sequential supernova explosionsoccurring during the lifetime of a giant molecular cloud.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "An overview of game-theoretic approaches to energy-efficient resourceallocation in wireless networks is presented. Focusing on multiple-accessnetworks, it is demonstrated that game theory can be used as an effective toolto study resource allocation in wireless networks with quality-of-service (QoS)constraints. A family of non-cooperative (distributed) games is presented inwhich each user seeks to choose a strategy that maximizes its own utility whilesatisfying its QoS requirements. The utility function considered here measuresthe number of reliable bits that are transmitted per joule of energy consumedand, hence, is particulary suitable for energy-constrained networks. Theactions available to each user in trying to maximize its own utility are atleast the choice of the transmit power and, depending on the situation, theuser may also be able to choose its transmission rate, modulation, packet size,multiuser receiver, multi-antenna processing algorithm, or carrier allocationstrategy. The best-response strategy and Nash equilibrium for each game ispresented. Using this game-theoretic framework, the effects of power control,rate control, modulation, temporal and spatial signal processing, carrierallocation strategy and delay QoS constraints on energy efficiency and networkcapacity are quantified.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The topological Tverberg theorem claims that for any continuous map of the(q-1)(d+1)-simplex to R^d there are q disjoint faces such that their imageshave a non-empty intersection. This has been proved for affine maps, and if $q$is a prime power, but not in general.  We extend the topological Tverberg theorem in the following way: Pairs ofvertices are forced to end up in different faces. This leads to the concept ofconstraint graphs. In Tverberg's theorem with constraints, we come up with alist of constraints graphs for the topological Tverberg theorem.  The proof is based on connectivity results of chessboard-type complexes.Moreover, Tverberg's theorem with constraints implies new lower bounds for thenumber of Tverberg partitions. As a consequence, we prove Sierksma's conjecturefor $d=2$, and $q=3$.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "A survey of Galactic gamma-ray sources at a median energy of ~20 TeV has beenperformed using the Milagro Gamma Ray Observatory. Eight candidate sources ofTeV emission are detected with pre-trials significance $>4.5\\sigma$ in theregion of Galactic longitude $l\\in[30^\\circ,220^\\circ]$ and latitude$b\\in[-10^\\circ,10^\\circ]$. Four of these sources, including the Crab nebulaand the recently published MGRO J2019+37, are observed with significances$>4\\sigma$ after accounting for the trials involved in searching the 3800square degree region. All four of these sources are also coincident with EGRETsources. Two of the lower significance sources are coincident with EGRETsources and one of these sources is Geminga. The other two candidates are inthe Cygnus region of the Galaxy. Several of the sources appear to be spatiallyextended. The fluxes of the sources at 20 TeV range from ~25% of the Crab fluxto nearly as bright as the Crab.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Trafficking of glutamate receptors into and out of synapses is criticallyinvolved in the plasticity of excitatory synaptic transmission. Endocytosis andexocytosis of receptors have initially been thought to account alone for thistrafficking. However, membrane proteins also traffic through surface lateraldiffusion in the plasma membrane. We describe developments inelectrophysiological and optical approaches that have allowed for the real timemeasurement of glutamate receptor surface trafficking in live neurons. Theseinclude (i) specific imaging of surface receptors using a pH sensitivefluorescent protein, (ii) design of a photoactivable drug to inactivate locallysurface receptors and monitor electrophysiologically their recovery, and(iii)application of single molecule fluorescence microscopy to directly trackthe movement of individual surface receptors with nanometer resolution insideand outside synapses. Altogether, these approaches have demonstrated thatglutamate receptors diffuse at high rates in the neuronal membrane and suggesta key role for surface diffusion in the regulation of receptor numbers atsynapses.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We propose a technique aimed at cooling a harmonically oscillating mirror toits quantum mechanical ground state starting from room temperature. Our method,which involves the two-sided irradiation of the vibrating mirror inside anoptical cavity, combines several advantages over the two-mirror arrangementsbeing used currently. For comparable parameters the three-mirror configurationprovides a stiffer trap for the oscillating mirror. Furthermore it preventsbistability from limiting the use of higher laser powers for mirror trapping,and also partially does so for mirror cooling. Lastly, it improves theisolation of the mirror from classical noise so that its dynamics are perturbedmostly by the vacuum fluctuations of the optical fields. These improvements areexpected to bring the task of achieving ground state occupation for the mirrorcloser to completion.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The astrometric signature imposed by a planet on its primary increasessubstantially towards longer periods (proportinal to P^2/3), so thatlong-period planets can be more easily detected, in principle. For example, aone Solar-mass (M_Sun) star would be pulled by roughly 1 mas by a oneJupiter-mass (M_J) planet with a period of one-hundred years at a distance of20 pc. Such position accuracies can now be obtained with both ground-based andspace-based telescopes. The difficulty was that it often takes many decadesbefore a detectable position shift will occur. However, by the time the nextgeneration of astrometric missions such as SIM will be taking data, severaldecades will have past since the first astrometric mission, HIPPARCOS. Here wepropose to use a new astrometric method that employs a future, highly accurateSIM Quick-Look survey and HIPPARCOS data taken twenty years prior. Usingposition errors for SIM of 4 muas, this method enables the detection andcharacterization of Solar-system analogs (SOSAs) with periods up to 240 (500)years for 1 (10) M_J companions. Because many tens of thousands nearby starscan be surveyed this way for a modest expenditure of SIM time and SOSAs may bequite abundant, we expect to find many hundreds of extra-solar planets withlong-period orbits. Such a data set would nicely complement the short-periodsystems found by the radial-velocity method. Brown dwarfs and low-mass stellarcompanions can be found and characterized if their periods are shorter thanabout 500 years. This data set will provide invaluable constraints on models ofplanet formation, as well as a database for systems where the location of thegiant planets allow for the formation of low-mass planets in the habitablezone. [Abridged]", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Charge ordering accompanied by lattice distortion in quasi-two dimensionalorganic conductors \\theta-(ET)2X (ET=BEDT-TTF) is studied by using an extendedHubbard model with Peierls-type electron-lattice couplings within theHartree-Fock approximation. It is found that the horizontal-stripecharge-ordered state, which is experimentally observed in\\theta-(ET)2RbZn(SCN)4, is stabilized by the self-consistently determinedlattice distortion. Furthermore, in the presence of the anisotropy innearest-neighbor Coulomb interactions Vij, the horizontal charge order becomesmore stable than any other charge patterns such as diagonal, vertical and3-fold-type states. At finite temperatures, we compare the free energies ofvarious charge-ordered states and find a first-order transition from a metallicstate with 3-fold charge order to the insulating state with the horizontalcharge order. The role of lattice degrees of freedom in the realization of thehorizontal charge order and the relevance to experiments on \\theta-(ET)2X arediscussed.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We experimentally investigate the temperature dependence of Rabi oscillationsand Ramsey fringes in superconducting phase qubits driven by microwave pulses.In a wide range of temperatures, we find that both the decay time and theamplitude of these coherent oscillations remain nearly unaffected by thermalfluctuations. The oscillations are observed well above the crossovertemperature from thermally activated escape to quantum tunneling for undrivenqubits. In the two-level limit, coherent qubit response rapidly vanishes assoon as the energy of thermal fluctuations kT becomes larger than the energylevel spacing of the qubit. Our observations shed new light on the origin ofdecoherence in superconducting qubits. The experimental data suggest that,without degrading already achieved coherence times, phase qubits can beoperated at temperatures much higher than those reported till now.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "One of the most surprising discoveries of extrasolar planets is the detectionof planets in moderately close binary star systems. The Jovian-type planets inthe two binaries of Gamma Cephei and GJ 86 have brought to the forefrontquestions on the formation of giant planets and the possibility of theexistence of smaller bodies in such dynamically complex environments. Thediverse dynamical characteristics of these objects have made scientists wonderto what extent the current theories of planet formation can be applied tobinaries and multiple star systems. At present, the sensitivity of thedetection techniques does not allow routine discovery of Earth-sized bodies inbinary systems. However, with the advancement of new techniques, and with therecent launch of CoRoT and the launch of Kepler in late 2008, the detection ofmore planets (possibly terrestrial-class objects) in such systems is on thehorizon. Theoretical studies and numerical modeling of terrestrial andhabitable planet formation are, therefore, necessary to gain fundamentalinsights into the prospects for life in such systems and have great strategicimpact on NASA science and missions.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Efficient injection of spin-polarized electrons into the conduction band ofsilicon is limited by the formation of a silicide at the ferromagnetic metal(FM)/silicon interface. In the present work, this \"magnetically-dead\" silicide(where strong spin-scattering significantly reduces injected spin polarization)is eliminated by moving the FM in the spin injector from the tunnel junctionbase anode to the emitter cathode and away from the silicon surface. Thisresults in over an order-of-magnitude increase in spin injection efficiency,from a previously-reported magnetocurrent ratio of ~2% to ~35% and an estimatedspin polarization in Si from ~1% to at least ~15%. The injector tunnel-junctionbias dependence of this spin transport signal is also measured, demonstratingthe importance of low bias voltage to preserve high injected spin polarization.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Braided quantum field theories proposed by Oeckl can provide a framework fordefining quantum field theories having Hopf algebra symmetries. In quantumfield theories, symmetries lead to non-perturbative relations among correlationfunctions. We discuss Hopf algebra symmetries and such relations in braidedquantum field theories. We give the four algebraic conditions between Hopfalgebra symmetries and braided quantum field theories, which are required forthe relations to hold. As concrete examples, we apply our discussions to thePoincare symmetries of two examples of noncommutative field theories. One isthe effective quantum field theory of three-dimensional quantum gravity coupledwith spinless particles given by Freidel and Livine, and the other isnoncommutative field theory on Moyal plane. We also comment on quantum fieldtheory on kappa-Minkowski spacetime.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We consider an electrostatic qubit, interacting with a fluctuating charge ofsingle electron transistor (SET) in the framework of exactly solvable model.The SET plays a role of the fluctuating environment affecting the qubit'sparameters in a controllable way. We derive the rate equations describingdynamics of the entire system for both weak and strong qubit-SET coupling.Solving these equation we obtain decoherence and relaxation rates of the qubit,as well as the spectral density of the fluctuating qubit's parameters. We foundthat in the weak coupling regime the decoherence and relaxation rates aredirectly related to the spectral density taken at Rabi or at zero frequency,depending on what a particular qubit's parameters is fluctuating. This relationholds also in the presence of weak back-action of the qubit on the fluctuatingenvironment. In the case of strong back-action, such simple relationship nolonger holds, even if the qubit-SET coupling is small. It does not hold eitherin the strong-coupling regime, even in the absence of the back-action. Inaddition, we found that our model predicts localization of the qubit in thestrong-coupling regime, resembling that of the spin-boson model.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Studying the internal structure of extragalactic jets is crucial forunderstanding their physics. The Japanese-led space VLBI project VSOP haspresented an opportunity for such studies, by reaching baseline lengths of upto 36,000 km and resolving structures down to an angular size of $\\approx 0.3$mas at 5 GHz. VSOP observations of the jet in 0836+710 at 1.6 and 5 GHz haveenabled tracing of the radial structure of the flow on scales from 2 mas to 200mas along the jet and determination of the wavelengths of individualoscillatory modes responsible for the formation of the structure observed. Weapply linear stability analysis to identify the oscillatory modes with modes ofKelvin-Helmholtz instability that match the wavelengths of the structuresobserved. We find that the jet structure in 0836+710 can be reproduced by thehelical surface mode and a combination of the helical and elliptic body modesof Kelvin-Helmholtz instability. Our results indicate that the jet issubstantially stratified and different modes of the instability grow inside thejet at different distances to the jet axis. The helical surface mode can bedriven externally, and we discuss the implications of the driving frequency onthe physics of the active nucleus in 0836+710.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Is it possible to understand cancer? Or more specifically, is it possible tounderstand cancer from genetic side? There already many answers in literature.The most optimistic one has claimed that it is mission-possible. Duesberg andhis colleagues reviewed the impressive amount of research results on canceraccumulated over 100 years. It confirms the a general opinion that consideringall available experimental results and clinical observations there is no cancertheory without major difficulties, including the prevailing gene-based cancertheories. They have then listed 9 \"absolute discrepancies\" for such cancertheory. In this letter the quantitative evidence against one of their majorreasons for dismissing mutation cancer theory, by both in vivo experiment and afirst principle computation, is explicitly pointed out.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "A combination of the memory function formalism and time-dependentdensity-functional theory is applied to transport in dilute magneticsemiconductors. The approach considers spin and charge disorder andelectron-electron interaction on an equal footing. Within the weak disorderlimit and using a simple parabolic approximation for the valence band we showthat Coulomb and exchange scattering contributions to the resistivity in GaMnAsare of the same order of magnitude. The positional correlations of defectsresult in a significant increase of Coulomb scattering, while the suppressionof localized spin fluctuations in the ferromagnetic phase contributessubstantially to the experimentally observed drop of resistivity below T_c. Aproper treatment of dynamical screening and collective excitations is essentialfor an accurate description of infrared absorption.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The operator-valued Schur-class is defined to be the set of holomorphicfunctions $S$ mapping the unit disk into the space of contraction operatorsbetween two Hilbert spaces. There are a number of alternate characterizations:the operator of multiplication by $S$ defines a contraction operator betweentwo Hardy Hilbert spaces, $S$ satisfies a von Neumann inequality, a certainoperator-valued kernel associated with $S$ is positive-definite, and $S$ can berealized as the transfer function of a dissipative (or even conservative)discrete-time linear input/state/output linear system. Various multivariablegeneralizations of this class have appeared recently,one of the mostencompassing being that of Muhly and Solel where the unit disk is replaced bythe strict unit ball of the elements of a dual correspondence $E^{\\sigma}$associated with a $W^{*}$-correspondence $E$ over a $W^{*}$-algebra $\\cA$together with a $*$-representation $\\sigma$ of $\\cA$. The main new point whichwe add here is the introduction of the notion of reproducing kernel Hilbertcorrespondence and identification of the Muhly-Solel Hardy spaces asreproducing kernel Hilbert correspondences associated with a completelypositive analogue of the classical Szeg\\\"o kernel. In this way we are able tomake the analogy between the Muhly-Solel Schur class and the classical Schurclass more complete. We also illustrate the theory by specializing it to somewell-studied special cases; in some instances there result new kinds ofrealization theorems.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "One of the goals of the landscape program in string theory is to extractinformation about the space of string vacua in the form of statisticalcorrelations between phenomenological features that are otherwise uncorrelatedin field theory. Such correlations would thus represent predictions of stringtheory that hold independently of a vacuum-selection principle. In this paper,we study statistical correlations between two features which are likely to becentral to any potential description of nature at high energy scales: gaugesymmetries and spacetime supersymmetry. We analyze correlations between thesetwo kinds of symmetry within the context of perturbative heterotic stringvacua, and find a number of striking features. We find, for example, that thedegree of spacetime supersymmetry is strongly correlated with the probabilitiesof realizing certain gauge groups, with unbroken supersymmetry at the stringscale tending to favor gauge-group factors with larger rank. We also find thatnearly half of the heterotic landscape is non-supersymmetric and yettachyon-free at tree level; indeed, less than a quarter of the tree-levelheterotic landscape exhibits any supersymmetry at all at the string scale.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "A large symmetry group is perhaps experimentally observed in excited hadronswhich includes the chiral group U(2)_L x U(2)_R as a subgroup. To possess thislarge symmetry a dynamical model for excited hadrons, presumably a stringmodel, should explain formation of chiral multiplets and, at the same time,predict coinciding slopes of the angular and radial Regge trajectories. This ispossible only if both the dynamics of the string and the chirality of thequarks at the ends of the string are considered together. We construct amodel-independent unitary transformation from the relativistic chiral basis tothe ^{2S+1}L_J basis, commonly used in hadronic phenomenology as well as in thestring models, and demonstrate that a hadron belonging to the given chiralrepresentation is a fixed superposition of the basis vectors with different L'sand S's. Thus the description of highly excited hadron in terms of a fixed L isnot compatible with chiral symmetry and has to be disregarded in favour of thedescription in terms of the total hadron spin J. Therefore, dynamics of thestring must deliver the principal quantum number ~n+J, in order chiralmultiplets with different spins to become degenerate, as required by the largesymmetry group.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "If dark matter decays to electromagnetically-interacting particles, it caninject energy into the baryonic gas and thus affect the processes ofrecombination and reionization. This leaves an imprint on the cosmic microwavebackground (CMB): the large-scale polarization is enhanced, and the small-scaletemperature fluctuation is damped. We use the WMAP three-year data combinedwith galaxy surveys to constrain radiatively decaying dark matter. Our newlimits to the dark-matter decay width are about ten times stronger thanprevious limits. For dark-matter lifetimes that exceed the age of the Universe,a limit of $\\zeta \\Gamma_{\\chi} < 1.7 \\times 10^{-25} s^{-1}$ (95% CL) isderived, where $\\zeta$ is the efficiency of converting decay energy intoionization energy. Limits for lifetimes short compared with the age of theUniverse are also derived. We forecast improvements expected from the Plancksatellite.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Superfluid 3He-A shares the properties of spin nematic and chiral orbitalferromagnet. Its order parameter is characterized by two vectors d and l. Thisdoubly anisotropic superfluid, when it is confined in aerogel, represents themost interesting example of a system with continuous symmetry in the presenceof random anisotropy disorder. We discuss the Larkin-Imry-Ma state, which ischaracterized by the short-range orientational order of the vector l, while thelong-range orientational order is destroyed by the collective action of therandomly oriented aerogel strings. On the other hand, sufficiently largeregular anisotropy produced either by the deformation of the aerogel or byapplied superflow suppresses the Larkin-Imry-Ma effect leading to the uniformorientation of the vector l. This interplay of regular and random anisotropyallows us to study many different effects.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The ever-increasing knowledge of the structure of various real-world networkshas uncovered their complex multi-mechanism-governed evolution processes.Therefore, a better understanding of the structure and evolution of thesenetworked complex systems requires us to describe such processes in a moredetailed and realistic manner. In this paper, we introduce a new type ofnetwork growth rule which comprises addition and deletion of nodes, and proposean evolving network model to investigate the effect of node deleting on networkstructure. It is found that, with the introduction of node deleting, networkstructure is significantly transformed. In particular, degree distribution ofthe network undergoes a transition from scale-free to exponential forms as theintensity of node deleting increases. At the same time, nontrivialdisassortative degree correlation develops spontaneously as a natural result ofnetwork evolution in the model. We also demonstrate that node deletingintroduced in the model does not destroy the connectedness of a growing networkso long as the increasing rate of edges is not excessively small. In addition,it is found that node deleting will weaken but not eliminate the small-worldeffect of a growing network, and generally it will decrease the clusteringcoefficient in a network.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The bandstructure was calculated by the full-potential linearized augmentedplane wave method. The result reveals two important insights to the novelsecond harmonic generation (SHG) of alpha-phase lithium iodate($\\alpha-LiIO_{3}$) crystal: the existence of finite intra-band momentum matrixelements due to the non-inversion symmetry of the crystal illuminating thepotential of the intra-band transition, and the strong covalent bonding betweenthe $I$-atoms and the ligand $O$-atoms resulting the condition of thedouble-resonance. An inter-band transition scenario in SHG as $\\alpha-LiIO_{3}$in nano-structure is proposed. The optical properties were calculated withinthe theoretical framework of the time-dependent perturbation of theindependent-particle model. The dielectric tensors and the refractive indexwere evaluated. Comparisons between the predictions and the results were made:the x-ray near edge absorption spectra; the refractive index at the staticlimit, and at finite frequencies. Possible factors attributing the calculationerrors is discussed.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "This paper analyses the possibilities of performing paralleltransaction-oriented simulations with a special focus on the space-parallelapproach and discrete event simulation synchronisation algorithms that aresuitable for transaction-oriented simulation and the target environment of AdHoc Grids. To demonstrate the findings a Java-based paralleltransaction-oriented simulator for the simulation language GPSS/H isimplemented on the basis of the promising Shock Resistant Time Warpsynchronisation algorithm and using the Grid framework ProActive. Thevalidation of this parallel simulator shows that the Shock Resistant Time Warpalgorithm can successfully reduce the number of rolled back Transaction movesbut it also reveals circumstances in which the Shock Resistant Time Warpalgorithm can be outperformed by the normal Time Warp algorithm. The conclusionof this paper suggests possible improvements to the Shock Resistant Time Warpalgorithm to avoid such problems.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We investigate an evolutional scenario of the FRW universe with the Casimirenergy scaling like $(-)(1+z)^4$. The Casimir effect is used to explain thevacuum energy differences (its value measured from astrophysics is so smallcompared to value obtained from quantum field theory calculations). Thedynamics of the FRW model is represented in terms of a two-dimensionaldynamical system to show all evolutional paths of this model in the phase spacefor all admissible initial conditions. We find also an exact solution for nonflat evolutional paths of Universe driven by the Casimir effect. The maindifference between the FRW model with the Casimir force and the $\\Lambda$CDMmodel is that their generic solutions are a set of evolutional paths with abounce solution and an initial singularity, respectively. The evolutionalscenario are tested by using the SNIa data, FRIIb radiogalaxies, baryonoscillation peak and CMB observation. We compare the power of explanation ofthe model considered and the $\\Lambda$CDM model using the Bayesian informationcriterion and Bayesian factor. Our investigation of the information criteria ofmodel selection showed the preference of the $\\Lambda$CDM model over the modelconsidered. However the presence of negative like the radiation term can removea tension between the theoretical and observed primordial ${}^4$He and Dabundance.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Although power laws of the Zipf type have been used by many workers to fitrank distributions in different fields like in economy, geophysics, genetics,soft-matter, networks etc., these fits usually fail at the tails. Somedistributions have been proposed to solve the problem, but unfortunately theydo not fit at the same time both ending tails. We show that many different datain rank laws, like in granular materials, codons, author impact in scientificjournal, etc. are very well fitted by a beta-like function. Then we proposethat such universality is due to the fact that a system made from manysubsystems or choices, imply stretched exponential frequency-rank functionswhich qualitatively and quantitatively can be fitted with the proposedbeta-like function distribution in the limit of many random variables. We provethis by transforming the problem into an algebraic one: finding the rank ofsuccessive products of a given set of numbers.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The photospheres of stars hosting planets have larger metallicity than starslacking planets. In the present work we study the possibility of an earliermetal enrichment of the photospheres by means of impacting planetesimals duringthe first 20-30Myr. Here we explore this contamination process by simulatingthe interactions of an inward migrating planet with a disc of planetesimalinterior to its orbit. The results show the percentage of planetesimals thatfall on the star. We identified the dependence of the planet's eccentricity($e_p$) and time scale of migration ($\\tau$) on the rate of infallingplanetesimals. For very fast migrations ($\\tau=10^2$yr and $\\tau=10^3$yr) thereis no capture in mean motion resonances, independently of the value of $e_p$.Then, due to the planet's migration the planetesimals suffer close approacheswith the planet and more than 80% of them are ejected from the system. For slowmigrations ($\\tau=10^5$yr and $\\tau=10^6$yr) the percentage of collisions withthe planet decrease with the increase of the planet's eccentricity. For $e_p=0$and $e_p=0.1$ most of the planetesimals were captured in the 2:1 resonance andmore than 65% of them collided with the star. Whereas migration of a Jupitermass planet to very short pericentric distances requires unrealistic high discmasses, these requirements are much smaller for smaller migrating planets. Oursimulations for a slowly migrating 0.1 $M_{\\rm Jupiter}$ planet, even demandinga possible primitive disc three times more massive than a primitive solarnebula, produces maximum [Fe/H] enrichments of the order of 0.18 dex. Thesecalculations open possibilities to explain hot Jupiters exoplanetsmetallicities.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The lowest-Landau-level anyon model becomes nonperiodic in the statisticsparameter when the finite size of the attached flux tubes is taken intoaccount. The finite-size effects cause the inverse proportional relationbetween the critical filling factor and the statistics parameter to benonperiodically continued in the screening regime, where the fluxes areanti-parallel to the external magnetic field -- at critical filling, theexternal magnetic field is entirely screened by the mean magnetic fieldassociated with the flux tubes. A clustering argument is proposed to selectparticular values of the statistics parameter. In this way, IQHE and FQHEfillings are obtained in terms of gapped nondegenerate LLL-anyonic wavefunctions. Jain's series are reproduced without the need to populate higherLandau levels. New FQHE series are proposed, like, in particular, theparticle-hole complementary series of the Laughlin one. For fast-rotatingBose-Einstein condensates, a corresponding clustering argument yieldsparticular fractional filling series.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Environmental dielectric screening effects on exciton transition energies insingle-walled carbon nanotubes (SWNTs) have been studied quantitatively in therange of dielectric constants from 1.0 to 37 by immersing SWNTs bridged overtrenches in various organic solvents by means of photoluminescence and theexcitation spectroscopies. With increasing environmental dielectric constant($\\epsilon_{\\rm env}$), both $E_{11}$ and $E_{22}$ exhibited a redshift byseveral tens meV and a tendency to saturate at a $\\epsilon_{\\rm env} \\sim 5$without an indication of significant ($n$,$m$) dependence. The redshifts can beexplained by dielectric screening of the repulsive electron-electroninteraction. The $\\epsilon_{\\rm env}$ dependence of $E_{11}$ and $E_{22}$ canbe expressed by a simple empirical equation with a power law in $\\epsilon_{\\rmenv}$, $E_{\\rm ii} = E_{\\rm ii}^{\\infty} + A\\epsilon_{\\rm env}^{-\\alpha}$. Wealso immersed a sample in sodium-dodecyl-sulfate (SDS) solution to investigatethe effects of wrapping SWNTs with surfactant. The resultant $E_{11}$ and$E_{22}$, which agree well with Weisman's data [Nano Lett. {\\bf 3}, 1235(2003)], are close to those of $\\epsilon_{\\rm env}$ of 2. However, in additionto the shift due to dielectric screening, another shift was observed so thatthe ($2n+m$)-family patterns spread more widely, similar to that of theuniaxial-stress-induced shift.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Magnetic nanoparticles with Neel surface anisotropy, different internalstructures, surface arrangements and elongation are modelled as many-spinsystems. The results suggest that the energy of many-spin nanoparticles cutfrom cubic lattices can be represented by an effective one-spin potentialcontaining uniaxial and cubic anisotropies. It is shown that the values andsigns of the corresponding constants depend strongly on the particle's surfacearrangement, internal structure and elongation. Particles cut from a simplecubic lattice have the opposite sign of the effective cubic term, as comparedto particles cut from the face-centered cubic lattice. Furthermore, otherremarkable phenomena are observed in nanoparticles with relatively strongsurface effects: (i) In elongated particles surface effects can change the signof the uniaxial anisotropy. (ii) In symmetric particles (spherical andtruncated octahedral) with cubic core anisotropy surface effects can change itssign. We also show that the competition between the core and surfaceanisotropies leads to a new energy that contributes to both the 2nd- and4th-order effective anisotropies.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "By generalizing and extending some of the earlier results derived by Maninand Merkulov, a twistor description is given of four-dimensional N-extended(gauged) self-dual supergravity with and without cosmological constant.Starting from the category of (4|4N)-dimensional complex superconformalsupermanifolds, the categories of (4|2N)-dimensional complex quaternionic,quaternionic Kaehler and hyper-Kaehler right-chiral supermanifolds areintroduced and discussed. We then present a detailed twistor description ofthese types of supermanifolds. In particular, we construct supertwistor spacesassociated with complex quaternionic right-chiral supermanifolds, and explainwhat additional supertwistor data allows for giving those supermanifolds ahyper-Kaehler structure. In this way, we obtain a supersymmetric generalizationof Penrose's nonlinear graviton construction. We furthermore give analternative formulation in terms of a supersymmetric extension of LeBrun'sEinstein bundle. This allows us to include the cases with nonvanishingcosmological constant. We also discuss the bundle of local supertwistors andaddress certain implications thereof. Finally, we comment on a real version ofthe theory related to Euclidean signature.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "In spite of the large number of papers appeared in the past which are devotedto the lattice Boltzmann (LB) methods, basic aspects of the theory still remainunchallenged. An unsolved theoretical issue is related to the construction of adiscrete kinetic theory which yields \\textit{exactly} the fluid equations,i.e., is non-asymptotic (here denoted as \\textit{LB inverse kinetic theory}).The purpose of this paper is theoretical and aims at developing an inversekinetic approach of this type. In principle infinite solutions exist to thisproblem but the freedom can be exploited in order to meet importantrequirements. In particular, the discrete kinetic theory can be defined so thatit yields exactly the fluid equation also for arbitrary non-equilibrium (butsuitably smooth) kinetic distribution functions and arbitrarily close to theboundary of the fluid domain. Unlike previous entropic LB methods the theoremcan be obtained without functional constraints on the class of the initialdistribution functions. Possible realizations of the theory and asymptoticapproximations are provided which permit to determine the fluid equations\\textit{with prescribed accuracy.} As a result, asymptotic accuracy estimatesof customary LB approaches and comparisons with the Chorin artificialcompressibility method are discussed.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "5972 independent and cumulative yields of radioactive residuals nuclei havebeen measured in 55 thin 206,207,208,nat-Pb and 209-Bi targets irradiated by0.04, 0.07, 0.10, 0.15, 0.25, 0.6, 0.8, 1.2, 1.4, 1.6, and 2.6 GeV protons.Besides, 219 yields have been measured in 0.3, 0.5, 0.75, 1.0, 1.5, and 2.6 GeVproton-irradiated 56-Fe target. The protons were extracted from the ITEP U-10synchrotron. The measured data are compared with experimental results obtainedelsewhere and with theoretical calculations by LAHET, MCNPX, CEM03, LAQGSM03,CASCADE, CASCADO, and LAHETO codes. The predictive power was found to bedifferent for each of the codes tested, but was satisfactory on the whole inthe case of spallation products. At the same time, none of the codes cande-scribe well the product yields throughout the whole product mass range, andall codes must be further improved.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We investigate the hydrodynamics of accretion channelled by a dipolarmagnetic field (funnel flows). We consider situations in which the electronsand ions in the flow cannot maintain thermal equilibrium (two-temperatureeffects) due to strong radiative loss, and determine the effects on the keVX-ray properties of the systems. We apply this model to investigate theaccretion shocks of white dwarfs in magnetic cataclysmic variables. We havefound that the incorporation of two-temperature effects could harden the keVX-rays. Also, the dipolar model yields harder X-ray spectra than the standardplanar model if white dwarf is sufficiently massive (>~1M_sun). When fittingobserved keV X-ray spectra of magnetic cataclysmic variables, the inclusion oftwo-temperature hydrodynamics and a dipolar accretion geometry lowers estimatesfor white-dwarf masses when compared with masses inferred from models excludingthese effects. We find mass reductions <~9% in the most massive cases.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "In this paper we study random induced subgraphs of the binary $n$-cube,$Q_2^n$. This random graph is obtained by selecting each $Q_2^n$-vertex withindependent probability $\\lambda_n$. Using a novel construction ofsubcomponents we study the largest component for$\\lambda_n=\\frac{1+\\chi_n}{n}$, where $\\epsilon\\ge \\chi_n\\ge n^{-{1/3}+\\delta}$, $\\delta>0$. We prove that there exists a.s. a unique largestcomponent $C_n^{(1)}$. We furthermore show that $\\chi_n=\\epsilon$, $|C_n^{(1)}|\\sim \\alpha(\\epsilon) \\frac{1+\\chi_n}{n} 2^n$ and for $o(1)=\\chi_n\\gen^{-{1/3}+\\delta}$, $| C_n^{(1)}| \\sim 2 \\chi_n \\frac{1+\\chi_n}{n} 2^n$ holds.This improves the result of \\cite{Bollobas:91} where constant $\\chi_n=\\chi$ isconsidered. In particular, in case of $\\lambda_n=\\frac{1+\\epsilon} {n}$, ouranalysis implies that a.s. a unique giant component exists.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We discuss Kondo behavior of a conduction electron system coupled with localoptical phonon by analyzing the Anderson-Holstein model with the use of anumerical renormalization group (NRG) method. There appear three typicalregions due to the balance between Coulomb interaction $U_{\\rm ee}$ andphonon-mediated attraction $U_{\\rm ph}$. For $U_{\\rm ee}>U_{\\rm ph}$, weobserve the standard Kondo effect concerning spin degree of freedom. Since theCoulomb interaction is effectively reduced as $U_{\\rm ee}-U_{\\rm ph}$, theKondo temperature $T_{\\rm K}$ is increased when $U_{\\rm ph}$ is increased. Onthe other hand, for $U_{\\rm ee}<U_{\\rm ph}$, there occurs the Kondo effectconcerning charge degree of freedom, since vacant and double occupied statesplay roles of pseudo-spins. Note that in this case, $T_{\\rm K}$ is decreasedwith the increase of $U_{\\rm ph}$. Namely, $T_{\\rm K}$ should be maximized for$U_{\\rm ee} \\approx U_{\\rm ph}$. Then, we analyze in detail the Kondo behaviorat $U_{\\rm ee}=U_{\\rm ph}$, which is found to be explained by the polaronAnderson model with reduced hybridization of polaron and residual repulsiveinteraction among polarons. By comparing the NRG results of the polaronAnderson model with those of the original Anderson-Holstein model, we clarifythe Kondo behavior in the competing region of $U_{\\rm ee} \\approx U_{\\rm ph}$.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "In object-oriented or object-relational databases such as multimediadatabases or most XML databases, access patterns are not static, i.e.,applications do not always access the same objects in the same orderrepeatedly. However, this has been the way these databases and associatedoptimisation techniques such as clustering have been evaluated up to now. Thispaper opens up research regarding this issue by proposing a dynamic objectevaluation framework (DOEF). DOEF accomplishes access pattern change bydefining configurable styles of change. It is a preliminary prototype that hasbeen designed to be open and fully extensible. Though originally designed forthe object-oriented model, it can also be used within the object-relationalmodel with few adaptations. Furthermore, new access pattern change models canbe added too. To illustrate the capabilities of DOEF, we conducted twodifferent sets of experiments. In the first set of experiments, we used DOEF tocompare the performances of four state of the art dynamic clusteringalgorithms. The results show that DOEF is effective at determining theadaptability of each dynamic clustering algorithm to changes in access pattern.They also led us to conclude that dynamic clustering algorithms can cope withmoderate levels of access pattern change, but that performance rapidly degradesto be worse than no clustering when vigorous styles of access pattern changeare applied. In the second set of experiments, we used DOEF to compare theperformance of two different object stores: Platypus and SHORE. The use of DOEFexposed the poor swapping performance of Platypus.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Multifrequency VLBA observations of the final group of ten objects in asample of FIRST-based compact steep spectrum (CSS) sources are presented. Thesample was selected to investigate whether objects of this kind could be relicsof radio-loud AGNs switched off at very early stages of their evolution orpossibly to indicate intermittent activity. Initial observations were madeusing MERLIN at 5 GHz. The sources have now been observed with the VLBA at 1.7,5 and 8.4 GHz in a snapshot mode with phase-referencing. The resulting maps arepresented along with unpublished 8.4-GHz VLA images of five sources. Some ofthe sources discussed here show a complex radio morphology and therefore acomplicated past that, in some cases, might indicate intermittent activity. Oneof the sources studied - 1045+352 - is known as a powerful radio andinfrared-luminous broad absorption line (BAL) quasar. It is a young CSS objectwhose asymmetric two-sided morphology on a scale of several hundred parsecs,extending in two different directions, may suggest intermittent activity. Theyoung age and compact structure of 1045+352 is consistent with the evolutionscenario of BAL quasars. It has also been confirmed that the submillimetre fluxof 1045+352 can be seriously contaminated by synchrotron emission.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Database search has wide applications and is used as a subroutine in manyimportant algorithms. We shall consider a database with one target item.Quantum algorithm finds the target item in a database faster than any classicalalgorithm. It frequently occurs in practice that only a portion of informationabout the target item is interesting, or we need to find a group of itemssharing some common feature as the target item. This problem is in generalformulated as search for a part of the database [a block] containing the targetitem, instead of the item itself. This is partial search. Partial search tradesaccuracy for speed, i.e. it works faster than a full search. Partial searchalgorithm was discovered by Grover and Radhakrishnan. We shall consideroptimized version of the algorithm and call it GRK. It can be appliedsuccessively [in a sequence]. First the database is partitioned into blocks andwe use GRK to find the target block. Then this target block is partitioned intosub-blocks and we use GRK again to find the target sub-block. [We can call itbinary quantum search.] Another possibility is to partition the database intosub-blocks directly and use GRK to find the target sub-block in one time. Inthis paper we prove that the latter is faster [makes less queries to theoracle].", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We compare the CO 2-1 observations against previously taken CO 4-3observations and analyze the spatial distribution of young stellar objects(YSO's) within the cloud using the Spitzer IRAC observations of the 30 Doraduscomplex. Both peaks of CO 2-1 and 4-3 emitting clouds coincide with the densestregion of the filaments where multiple shells are colliding. We find that theYSO's are clustered in the southern ridge of the warm and dense molecular gasclouds traced by CO J=4-3, indicating a filamentary structure of star formationthroughout the 30 Doradus. We also find that some of Class I YSO's candidateswhich are likely to be associated with a high-velocity component of CO 4-3emitting clouds are present. This is a bona fide place where the triggered starformation had happened and newly formed stars may have produced such ahigh-velocity outflow interacting with the surrounding molecular cloudmaterial.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present ACS/HST coronagraphic observations of HD 100546, a B9.5 star, 103pc away from the sun, taken in the F435W, F606W, and F814W bands. Scatteredlight is detected up to 14'' from the star. The observations are consistentwith the presence of an extended flattened nebula with the same inclination asthe inner disk. The well-known ``spiral arms'' are clearly observed and theytrail the rotating disk material. Weaker arms never before reported are alsoseen. The inter-arm space becomes brighter, but the structures become moreneutral in color at longer wavelengths, which is not consistent with modelsthat assume that they are due to the effects of a warped disk. Along the majordisk axis, the colors of the scattered-light relative to the star are \\Delta(F435W-F606W) ~ 0.0--0.2 mags and \\Delta (F435W-F814W)~0.5--1 mags. To explainthese colors, we explore the role of asymmetric scattering, reddening, andlarge minimum sizes on ISM-like grains. We conclude each of these hypotheses byitself cannot explain the colors. The disk colors are similar to those derivedfor Kuiper Belt objects, suggesting that the same processes responsible fortheir colors may be at work here. We argue that we are observing only thegeometrically thick, optically thin envelope of the disk, while the opticallythick disk responsible for the far-IR emission is undetected. The observedspiral arms are then structures on this envelope. The colors indicate that theextended nebulosity is not a remnant of the infalling envelope but reprocesseddisk material.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We conducted a preliminary field study to understand the current state ofpersonal digital archiving in practice. Our aim is to design a service for thelong-term storage, preservation, and access of digital belongings by examininghow personal archiving needs intersect with existing and emerging archivingtechnologies, best practices, and policies. Our findings not only confirmedthat experienced home computer users are creating, receiving, and finding anincreasing number of digital belongings, but also that they have already lostirreplaceable digital artifacts such as photos, creative efforts, and records.Although participants reported strategies such as backup and file replicationfor digital safekeeping, they were seldom able to implement them consistently.Four central archiving themes emerged from the data: (1) people find itdifficult to evaluate the worth of accumulated materials; (2) personal storageis highly distributed both on- and offline; (3) people are experiencingmagnified curatorial problems associated with managing files in the aggregate,creating appropriate metadata, and migrating materials to maintainable formats;and (4) facilities for long-term access are not supported by the currentdesktop metaphor. Four environmental factors further complicate archiving inconsumer settings: the pervasive influence of malware; consumer reliance on adhoc IT providers; an accretion of minor system and registry inconsistencies;and strong consumer beliefs about the incorruptibility of digital forms, thereliability of digital technologies, and the social vulnerability of networkedstorage.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We investigate the mass function in the substellar domain down to a fewJupiter masses in the young sigma Orionis open cluster (3+/-2 Ma, d =360^+70_-60 pc). We have performed a deep IJ-band search, covering an area of790 arcmin^2 close to the cluster centre. This survey was complemented with aninfrared follow-up in the HKs- and Spitzer 3.6-8.0 mum-bands. Usingcolour-magnitude diagrams, we have selected 49 candidate cluster members in themagnitude interval 16.1 mag < I < 23.0 mag. Accounting for flux excesses at 8.0mum and previously known spectral features of youth, 30 objects are bona fidecluster members. Four are first identified from our optical-near infrared data.Eleven have most probable masses below the deuterium burning limit and areclassified as planetary-mass object candidates. The slope of the substellarmass spectrum (Delta N / Delta M = a M^-alpha) in the mass interval 0.11 Msol M< 0.006 Msol is alpha = +0.6+/-0.2. Any opacity mass-limit, if these objectsform via fragmentation, may lie below 0.006 Msol. The frequency of sigmaOrionis brown dwarfs with circumsubstellar discs is 47+/-15 %. The continuityin the mass function and in the frequency of discs suggests that very low-massstars and substellar objects, even below the deuterium-burning mass limit, mayshare the same formation mechanism.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We consider that the pre-inflation era is radiation-dominated, transitingsmoothly to the inflationary era. We work out in detail the dynamics ofinflaton fluctuations across the phase transition and the proper choices ofinitial vacuum states. It is found that this phase transition can suppresslong-wavelength quantum fluctuations of inflaton. This may attribute to thelarge-scale CMB anisotropy a lower power than predicted in the standard$\\Lambda$CDM model. In constraining this transitional effect by WMAP anisotropydata, we use the WMAP best-fit scale-invariant $\\Lambda$CDM model with thedensity power spectrum replaced by the one found in this work. We find that thetransition occurs at least about 10 e-folds before the comoving scalescomparable to our present horizon size cross the Hubble radius duringinflation.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "This paper extends and builds upon the results of an earlier paper, in whichwe described how to use the tools of geometrical engineering to deformgeometrically-engineered grand unified models into ones with lower symmetry.This top-down unfolding has the advantage that the relative positions ofsingularities giving rise to the many `low energy' matter fields are related byonly a few parameters which deform the geometry of the unified model. Andbecause the relative positions of singularities are necessary to compute thesuperpotential, for example, this is a framework in which the arbitrariness ofgeometrically engineered models can be greatly reduced.  In our earlier paper, this picture was made concrete for the case ofdeforming the representations of an SU(5) model into their Standard Modelcontent. In this paper we continue that discussion to show how a geometricallyengineered 16 of SO(10) can be unfolded into the Standard Model, and how thethree families of the Standard Model uniquely emerge from the unfolding of asingle, isolated E8 singularity.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "[Abridged] We have been exploring a spectroscopic unification for all knowntypes of broad line emitting AGN. The 4D Eigenvector 1 (4DE1) parameter spaceshows promise as a unification capable of organizing quasar diversity on asequence primarily governed by Eddington ratio. This paper considers the roleof CIV 1549 measures with special emphasis on the CIV 1549 line shift as aprincipal 4DE1 diagnostic. We use HST archival spectra for 130 sources with S/Nhigh enough to permit reliable CIV 1549 broad component (BC) measures. We finda CIV 1549 BC profile blueshift that is strongly concentrated among (largelyradio-quiet: RQ) sources with FWHM(H beta BC) < 4000 km/s (which we callPopulation A). Narrow line Seyfert 1 (NLSy1, with FWHM H beta < 2000 km/s)sources belong to this population but do not emerge as a distinct class. Thesystematic blueshift, widely interpreted as arising in a disk wind/outflow, isnot observed in broader lined AGN which we call Population B. We find newcorrelations between FWHM(CIV 1549 BC) and CIV 1549 line shift as well as theequivalent width of CIV 1549. They are seen only in Pop. A sources. CIV 1549measures enhance the apparent dichotomy at FWHM(Hbeta BC) approx. 4000 \\kms\\(Sulentic et al. 2000) suggesting that it has more significance in the contextof Broad Line Region structure than the more commonly discussed RL vs. RQdichotomy. Black hole masses computed from FWHM CIV 1549 BC for about 80 AGNindicate that the CIV 1549 width is a poor virial estimator. Comparison of massestimates derived from Hbeta BC and CIV 1549 reveals that the latter showdifferent and nonlinear offsets for population A and B sources. A significantnumber of sources also show narrow line CIV 1549 emission. We present a recipefor CIV 1549 narrow component extraction.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "In the radio regime the mass-loss rate of AGB stars is best probed usingmolecular (and atomic) line emission arising in the CSE formed by the stellarwind. The numerical modelling of the circumstellar emission where intricateinterplays between physical and chemical processes take place, is a challenge.The derived mass-loss rates depend crucially on the assumptions in thecircumstellar model, of which some can be constrained if enough observationaldata exist. Therefore, a reliable mass-loss-rate determination for anindividual star requires, in addition to a detailed radiative transferanalysis, good observational constraints in the form of multi-line observationsand radial brightness distributions. Of the methods used to estimate mass-lossrates from galactic AGB stars those based on radiative transfer modelling of COline emission are most commonly used and possibly also the most accurate.Typically, CO multi-transitional observations can constrain the mass-loss rateto better than 50%, within the adopted circumstellar model. Comparison withcomplementary methods, such as estimates based on dust radiative transfermodelling coupled with a dynamical model, are consistent within a factor ofthree.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "AU Pegasi is a pulsating star in a spectroscopic binary system with anorbital period of 53.26 days. Between 1960 and 1990 an extremely rapid periodincrease was observed in the value of the pulsation period, but in the last 15years the observation show that the period set in 2.411 days. Fourier analysisof photometric data obtained during the ASAS project and those taken at thePiszkesteto Mountain Station of the Konkoly Observatory during 1994-2005indicate that AU Pegasi is pulsating in two modes simultaneously, and the ratioof the frequencies of the two modes is 0.706, a value common for double-modeclassical Cepheids. A careful analysis of other photometric observationsobtained during the era of the strong period increase also revealed existenceof a second mode. This may suggest that this star is not a Type II Cepheid,despite its galactic position.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We prove that every complete connected immersed surface with positiveextrinsic curvature $K$ in $H^2\\times R$ must be properly embedded,homeomorphic to a sphere or a plane and, in the latter case, study the behaviorof the end. Then, we focus our attention on surfaces with positive constantextrinsic curvature ($K-$surfaces). We establish that the only complete$K-$surfaces in $S^2\\times R$ and $H^2\\times R$ are rotational spheres. Hereare the key steps to achieve this. First height estimates for compact$K-$surfaces in a general ambient space $M^2\\times R$ with boundary in a sliceare obtained. Then distance estimates for compact $K-$surfaces (andH-$surfaces) in $H^2\\times R$ with boundary on a vertical plane are obtained.Finally we construct a quadratic form with isolated zeroes of negative index.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We apply a recently developed perturbative formalism which describes theevolution under their self-gravity of particles displaced from a perfectlattice to quantify precisely, up to shell crossing, the effects ofdiscreteness in dissipationless cosmological N-body simulations. We give simpleexpressions, explicitly dependent on the particle density, for the evolution ofpower in each mode as a function of red-shift. For typical starting red-shiftsthe effect of finite particle number is to {\\it slow down} slightly the growthof power compared to that in the fluid limit (e.g. by about ten percent at halfthe Nyquist frequency), and to induce also dispersion in the growth as afunction of direction at a comparable level. In the limit that the initialred-shift tends to infinity, at fixed particle density, the evolution in factdiverges from that in the fluid limit (described by the Zeldovichapproximation). Contrary to widely held belief, this means that a simulationstarted at a red-shift much higher than the red-shift of shell crossingactually gives a worse, rather than a better, result. We also study how theseeffects are modified when there is a small-scale regularization of thegravitational force. We show that such a smoothing may reduce the anisotropy ofthe discreteness effects, but it then {\\it increases} their average effect.This behaviour illustrates the fact that the discreteness effects describedhere are distinct from those usually considered in this context, due totwo-body collisions. Indeed the characteristic time for divergence from thecollisionless limit is proportional to $N^{2/3}$, rather than $N/ \\log N$ inthe latter case.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We report quantitative relations between corruption level and economicfactors, such as country wealth and foreign investment per capita, which arecharacterized by a power law spanning multiple scales of wealth and investmentsper capita. These relations hold for diverse countries, and also remain stableover different time periods. We also observe a negative correlation betweenlevel of corruption and long-term economic growth. We find similar results fortwo independent indices of corruption, suggesting that the relation betweencorruption and wealth does not depend on the specific measure of corruption.The functional relations we report have implications when assessing therelative level of corruption for two countries with comparable wealth, and forquantifying the impact of corruption on economic growth and foreigninvestments.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We study the properties of the Heisenberg antiferromagnet with spatiallyanisotropic nearest-neighbour exchange couplings on the kagome net, i.e. withcoupling J in one lattice direction and couplings J' along the other twodirections. For J/J' > 1, this model is believed to describe the magneticproperties of the mineral volborthite. In the classical limit, it exhibits twokinds of ground states: a ferrimagnetic state for J/J' < 1/2 and a largemanifold of canted spin states for J/J' > 1/2. To include quantum effectsself-consistently, we investigate the Sp(N) symmetric generalisation of theoriginal SU(2) symmetric model in the large-N limit. In addition to thedependence on the anisotropy, the Sp(N) symmetric model depends on a parameterkappa that measures the importance of quantum effects. Our numericalcalculations reveal that in the kappa-J/J' plane, the system shows a rich phasediagram containing a ferrimagnetic phase, an incommensurate phase, and adecoupled chain phase, the latter two with short- and long-range order. Wecorroborate these results by showing that the boundaries between the variousphases and several other features of the Sp(N) phase diagram can be determinedby analytical calculations. Finally, the application of a block-spinperturbation expansion to the trimerised version of the original spin-1/2 modelleads us to suggest that in the limit of strong anisotropy, J/J' >> 1, theground state of the original model is a collinearly ordered antiferromagnet,which is separated from the incommensurate state by a quantum phase transition.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We propose a model based on SU(5) x {}^{(d)}T which successfully gives riseto near tri-bimaximal leptonic mixing as well as realistic CKM matrix elementsfor the quarks. The Georgi-Jarlskog relations for three generations are alsoobtained. Due to the {}^{(d)}T transformation property of the matter fields,the b-quark mass can be generated only when the {}^{(d)}T symmetry is broken,giving a dynamical origin for the hierarchy between m_{b} and m_{t}. There areonly nine operators allowed in the Yukawa sector up to at least mass dimensionseven due to an additional Z_{12} x Z'_{12} symmetry, which also forbids, up tosome high orders, operators that lead to proton decay. The resulting model hasa total of nine parameters in the charged fermion and neutrino sectors, andhence is very predictive. In addition to the prediction for \\theta_{13} \\simeq\\theta_{c}/3 \\sqrt{2}, the model gives rise to a sum rule,\\tan^{2}\\theta_{\\odot} \\simeq \\tan^{2} \\theta_{\\odot, \\mathrm{TBM}} - {1/2}\\theta_{c} \\cos\\beta, which is a consequence of the Georgi-Jarlskog relationsin the quark sector. This deviation could account for the difference betweenthe experimental best fit value for the solar mixing angle and the valuepredicted by the tri-bimaximal mixing matrix.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We model the interaction between the wind from a newly formed rapidlyrotating magnetar and the surrounding supernova shock and host star. Thedynamics is modeled using the two-dimensional, axisymmetric thin-shellequations. In the first ~10-100 seconds after core collapse the magnetarinflates a bubble of plasma and magnetic fields behind the supernova shock. Thebubble expands asymmetrically because of the pinching effect of the toroidalmagnetic field, just as in the analogous problem of the evolution of pulsarwind nebulae. The degree of asymmetry depends on E_mag/E_tot. The correct valueof E_mag/E_tot is uncertain because of uncertainties in the conversion ofmagnetic energy into kinetic energy at large radii in relativistic winds; weargue, however, that bubbles inflated by newly formed magnetars are likely tobe significantly more magnetized than their pulsar counterparts. We show thatfor a ratio of magnetic to total power supplied by the central magnetarL_mag/L_tot ~ 0.1 the bubble expands relatively spherically. For L_mag/L_tot ~0.3, however, most of the pressure in the bubble is exerted close to therotation axis, driving a collimated outflow out through the host star. This canaccount for the collimation inferred from observations of long-durationgamma-ray bursts (GRBs). Outflows from magnetars become increasinglymagnetically dominated at late times, due to the decrease in neutrino-drivenmass loss as the young neutron star cools. We thus suggest that themagnetar-driven bubble initially expands relatively spherically, enhancing theenergy of the associated supernova, while at late times it becomesprogressively more collimated, producing the GRB.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We analyse and compare the complexity of several algorithms for computingmodular polynomials. We show that an algorithm relying on floating pointevaluation of modular functions and on interpolation, which has received littleattention in the literature, has a complexity that is essentially (up tologarithmic factors) linear in the size of the computed polynomials. Inparticular, it obtains the classical modular polynomials $\\Phi_\\ell$ of primelevel $\\ell$ in time O (\\ell^3 \\log^4 \\ell \\log \\log \\ell). Besides treatingmodular polynomials for $\\Gamma^0 (\\ell)$, which are an important ingredient inmany algorithms dealing with isogenies of elliptic curves, the algorithm iseasily adapted to more general situations. Composite levels are handled just aseasily as prime levels, as well as polynomials between a modular function andits transform of prime level, such as the Schl\\\"afli polynomials and theirgeneralisations. Our distributed implementation of the algorithm confirms thetheoretical analysis by computing modular equations of record level around10000 in less than two weeks on ten processors.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We considered diffusion-driven processes on small-world networks withdistance-dependent random links. The study of diffusion on such networks ismotivated by transport on randomly folded polymer chains, synchronizationproblems in task-completion networks, and gradient driven transport onnetworks. Changing the parameters of the distance-dependence, we found a richphase diagram, with different transient and recurrent phases in the context ofrandom walks on networks. We performed the calculations in two limiting cases:in the annealed case, where the rearrangement of the random links is fast, andin the quenched case, where the link rearrangement is slow compared to themotion of the random walker or the surface. It has been well-established thatin a large class of interacting systems, adding an arbitrarily small densityof, possibly long-range, quenched random links to a regular lattice interactiontopology, will give rise to mean-field (or annealed) like behavior. In somecases, however, mean-field scaling breaks down, such as in diffusion or in theEdwards-Wilkinson process in \"low-dimensional\" small-world networks. Thisbreak-down can be understood by treating the random links perturbatively, wherethe mean-field (or annealed) prediction appears as the lowest-order term of anaive perturbation expansion. The asymptotic analytic results are alsoconfirmed numerically by employing exact numerical diagonalization of thenetwork Laplacian. Further, we construct a finite-size scaling framework forthe relevant observables, capturing the cross-over behaviors in finitenetworks. This work provides a detailed account of theself-consistent-perturbative and renormalization approaches briefly introducedin two earlier short reports.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The paper considers pseudo-differential boundary value control systems. Theunderlying operators form an algebra D with the help of which we are able toformulate typical boundary value control problems. The symbolic calculus givestools to form e.g. compositions, formal adjoints, generalized right or leftinverses and compatibility conditions. By a parametrizability we mean that fora given control system Au=0 one finds an operator S such that Au=0 if and onlyif u=Sf. The computation rules of D (or its appropriate subalgebra D')guarantee that in many applications S can be refinely analyzed or evenexplicitly calculated. We outline some methods of homological algebra for thestudy of parametrization S. Especially the projectivity of a certain factormodule (defined by the system equations) implies the parametrizability. We givesome examples to illustrate our computational methods.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "This work reports a theoretical study of the gas phase unimoleculardecomposition of cyclobutane, cyclopentane and cyclohexane by means of quantumchemical calculations. A biradical mechanism has been envisaged for eachcycloalkane, and the main routes for the decomposition of the biradicals formedhave been investigated at the CBS-QB3 level of theory. Thermochemical data(\\delta H^0_f, S^0, C^0_p) for all the involved species have been obtained bymeans of isodesmic reactions. The contribution of hindered rotors has also beenincluded. Activation barriers of each reaction have been analyzed to assess the1 energetically most favorable pathways for the decomposition of biradicals.Rate constants have been derived for all elementary reactions using transitionstate theory at 1 atm and temperatures ranging from 600 to 2000 K. Global rateconstant for the decomposition of the cyclic alkanes in molecular products havebeen calculated. Comparison between calculated and experimental results allowedto validate the theoretical approach. An important result is that therotational barriers between the conformers, which are usually neglected, are ofimportance in decomposition rate of the largest biradicals. Ring strainenergies (RSE) in transition states for ring opening have been estimated andshow that the main part of RSE contained in the cyclic reactants is removedupon the activation process.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The Special Theory of Relativity and the Theory of the Electron have had aninteresting history together. Originally the electron was studied in a nonrelativistic context and this opened up the interesting possibility that leadto the conclusion that the mass of the electron could be thought of entirely inelectromagnetic terms without introducing inertial considerations. However theapplication of Special Relativity lead to several problems, both for anextended electron and the point electron. These inconsistencies have, contraryto popular belief not been resolved satisfactorily today, even within thecontext of Quantum Theory. Nevertheless these and subsequent studies bring outthe interesting result that Special Relativity breaks down within the Comptonscale or when the Compton scale is not neglected. This again runs contrary toan uncritical notion that Special Relativity is valid for point particles.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We have conducted a high-resolution ``3D'' imaging survey of the CO(1--0),HCN(1--0), and HCO$^+$(1--0) lines toward the central a few kpc regions of theSeyfert and starburst galaxies in the local universe using the NobeyamaMillimeter Array. We detected luminous HCN(1--0) emissions toward aconsiderable fraction of these Seyfert galaxies (10 of 12 in our sub-sample),which indicated that some of these Seyfert galaxies, such as NGC 3079, NGC3227, NGC 4051, NGC 6764, and NGC 7479, are indeed accompanied with compactnuclear starburst, given the tight correlation between the HCN(1--0) luminosityand the star formation rate among star-forming galaxies. However, we suggestthat the elevated HCN(1--0) emission from some of these Seyfert galaxies,including NGC 1068, NGC 1097, NGC 5033, and NGC 5194, does not signify thepresence of massive starbursts there. This is because these Seyfert nuclei showabnormally high HCN(1--0)/HCO$^+$(1--0) ratios (2--3), which were neverobserved in the starburst nuclei in our sample. This could be attributed to theoverabundance of HCN molecules in the X-ray dominated regions (XDRs) at thecenters of these Seyfert galaxies.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Cornell University, the California Institute for Technology, and the JetPropulsion Laboratory are jointly studying the construction of a 25 m diametertelescope for submillimeter astronomy on a high mountain in northern Chile.This Cornell Caltech Atacama Telescope (CCAT) will combine high sensitivity, awide field of view, and a broad wavelength range to provide an unprecedentedcapability for deep, large area, multi-color submillimeter surveys tocomplement narrow field, high resolution studies with ALMA. CCAT observationswill address fundamental themes in contemporary astronomy, notably theformation and evolution of galaxies, the nature of the dark matter and darkenergy that comprise most of the content of the universe, the formation ofstars and planets, the conditions in circumstellar disks, and the conditionsduring the early history of the Solar system. The candidate CCAT site, at 5600m in northern Chile, enjoys superb observing conditions. To accommodate largeformat bolometer cameras, CCAT is designed with a 20 arcmin field of view. CCATwill incorporate closed loop active control of its segmented primary mirror tomaintain a half wavefront error of 10 mum rms or less. Instrumentation underconsideration includes both short (650 mum-200 mum) and long (2 mm-750 mum)wavelength bolometer cameras, direct detection spectrometers, and heterodynereceiver arrays. The University of Colorado, a Canadian university consortium,and the UK Astronomy Technology Centre on behalf of the UK community arepursuing participation in the CCAT consortium. When complete early in the nextdecade, CCAT will be the largest and most sensitive facility of its class aswell as the highest altitude astronomical facility on Earth.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The Naval Research Laboratory and the National Radio Astronomy Observatorycompleted implementation of a low frequency capability on the VLA at 73.8 MHzin 1998. This frequency band offers unprecedented sensitivity (~25 mJy/beam)and resolution (~25 arcsec) for low-frequency observations. We review thehardware, the calibration and imaging strategies, comparing them to those athigher frequencies, including aspects of interference excision and wide-fieldimaging. Ionospheric phase fluctuations pose the major difficulty incalibrating the array. Over restricted fields of view or at times of extremelyquiescent ionospheric ``weather'', an angle-invariant calibration strategy canbe used. In this approach a single phase correction is devised for eachantenna, typically via self-calibration. Over larger fields of view or at timesof more normal ionospheric ``weather'' when the ionospheric isoplanatic patchsize is smaller than the field of view, we adopt a field-based strategy inwhich the phase correction depends upon location within the field of view. Thissecond calibration strategy was implemented by modeling the ionosphere abovethe array using Zernike polynomials. Images of 3C sources of moderate strengthare provided as examples of routine, angle-invariant calibration and imaging.Flux density measurements indicate that the 74 MHz flux scale at the VLA isstable to a few percent, and tied to the Baars et al. value of Cygnus A at the5 percent level. We also present an example of a wide-field image, devoid ofbright objects and containing hundreds of weaker sources, constructed from thefield-based calibration. We close with a summary of lessons the 74 MHz systemoffers as a model for new and developing low-frequency telescopes. (Abridged)", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Experimental studies have shown the ubiquity of altruistic behavior in humansocieties. The social structure is a fundamental ingredient to understand thedegree of altruism displayed by the members of a society, in contrast toindividual-based features, like for example age or gender, which have beenshown not to be relevant to determine the level of altruistic behavior. Weexplore an evolutionary model aiming to delve how altruistic behavior isaffected by social structure. We investigate the dynamics of interactingindividuals playing the Ultimatum Game with their neighbors given by a socialnetwork of interaction. We show that a population self-organizes in a criticalstate where the degree of altruism depends on the topology characterizing thesocial structure. In general, individuals offering large shares but in turnaccepting large shares, are removed from the population. In heterogeneoussocial networks, individuals offering intermediate shares are strongly selectedin contrast to random homogeneous networks where a broad range of offers, belowa critical one, is similarly present in the population.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present the results of the analysis of neutrino observations by theAntarctic Muon and Neutrino Detector Array (AMANDA) correlated with photonobservations of more than 400 gamma-ray bursts (GRBs) in the NorthernHemisphere from 1997 to 2003. During this time period, AMANDA's effectivecollection area for muon neutrinos was larger than that of any other existingdetector. Based on our observations of zero neutrinos during and immediatelyprior to the GRBs in the dataset, we set the most stringent upper limit on muonneutrino emission correlated with gamma-ray bursts. Assuming a Waxman-Bahcallspectrum and incorporating all systematic uncertainties, our flux upper limithas a normalization at 1 PeV of  E^2{\\Phi}_{\\nu} {\\leq} 6.0 \\times 10^{-9} GeV cm^{-2} s^{-1} sr^{-1}, with90% of the events expected within the energy range of ~10 TeV to ~3 PeV. Theimpact of this limit on several theoretical models of GRBs is discussed, aswell as the future potential for detection of GRBs by next generation neutrinotelescopes. Finally, we briefly describe several modifications to this analysisin order to apply it to other types of transient point sources.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The churn rate of a peer-to-peer system places direct limitations on the rateat which messages can be effectively communicated to a group of peers. Theselimitations are independent of the topology and message transmission latency.In this paper we consider a peer-to-peer network, based on the Engset model,where peers arrive and depart independently at random. We show how the arrivaland departure rates directly limit the capacity for message streams to bebroadcast to all other peers, by deriving mean field models that accuratelydescribe the system behavior. Our models cover the unit and more general kbuffer cases, i.e. where a peer can buffer at most k messages at any one time,and we give results for both single and multi-source message streams. We definecoverage rate as peer-messages per unit time, i.e. the rate at which a numberof peers receive messages, and show that the coverage rate is limited by thechurn rate and buffer size. Our theory introduces an Instantaneous MessageExchange (IME) model and provides a template for further analysis of morecomplicated systems. Using the IME model, and assuming random processes, wehave obtained very accurate equations of the system dynamics in a variety ofinteresting cases, that allow us to tune a peer-to-peer system. It remains tobe seen if we can maintain this accuracy for general processes and whenapplying a non-instantaneous model.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The cosmological redshift phenomenon can be described by the dark matterfield fluid model, the results deduced from this model agree very well with theobservations. The observed cosmological redshift of light depends on both thespeed of the emitter and the distance between the emitter and the observer. Ifthe emitter moves away from us, a redshift is observed. If the emitter movestowards us, whether a redshift, a blueshift or no shift is observed will dependon the speed vs. the distance. If the speed is in the range ofc(exp[-beta*D]-1) < v < 0, a redshift is observed; if the speed equalsc(exp[-beta*D]-1), no shift is observed; if the speed v less thanc(exp[-beta*D]-1), a blueshift is observed. A redshift will be always observedin all directions for any celestial objects as long as their distance from usis large enough. Therefore, many more redshifts than blueshifts should beobserved for galaxies and supernovae, etc in the sky. This conclusion agreeswith current observations. The estimated value of the redshift constant beta ofthe dark matter field fluid is in the range of 10^(-3) ~ 10^(-5)/Mpc. A largeredshift value from a distant celestial object may not necessarily indicatethat it has a large receding speed. Based on the redshift effect of dark matterfield fluid, it is concluded that at least in time average all photons have thesame geometry (size and shape) in all inertial reference frames and do not havelength contraction effect.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Redundancy of experimental data is the basic statistic from which thecomplexity of a natural phenomenon and the proper number of experiments neededfor its exploration can be estimated. The redundancy is expressed by theentropy of information pertaining to the probability density function ofexperimental variables. Since the calculation of entropy is inconvenient due tointegration over a range of variables, an approximate expression for redundancyis derived that includes only a sum over the set of experimental data aboutthese variables. The approximation makes feasible an efficient estimation ofthe redundancy of data along with the related experimental information andinformation cost function. From the experimental information the complexity ofthe phenomenon can be simply estimated, while the proper number of experimentsneeded for its exploration can be determined from the minimum of the costfunction. The performance of the approximate estimation of these statistics isdemonstrated on two-dimensional normally distributed random data.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Finite metric trees are known to have strict 1-negative type. In this paperwe introduce a new family of inequalities that quantify the extent of the\"strictness\" of the 1-negative type inequalities for finite metric trees. Theseinequalities of \"enhanced 1-negative type\" are sufficiently strong to implythat any given finite metric tree must have strict p-negative type for allvalues of p in an open interval that contains the number 1. Moreover, theseopen intervals can be characterized purely in terms of the unordereddistribution of edge weights that determine the path metric on the particulartree, and are therefore largely independent of the tree's internal geometry.  From these calculations we are able to extract a new non linear technique forimproving lower bounds on the maximal p-negative type of certain finite metricspaces. Some pathological examples are also considered in order to stresscertain technical points.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "This paper focuses on the kinematic properties of a newthree-degree-of-freedom hybrid manipulator. This manipulator is obtained byadding in series to a five-bar planar mechanism (similar to the one studied byBajpai and Roth) a third revolute passing through the line of centers of thetwo actuated revolute joints of the above linkage. The resulting architectureis hybrid in that it has both serial and parallel links. Fully-parallelmanipulators are known for the existence of particularly undesirablesingularities (referred to as parallel singularities) where control is lost [4]and [6]. On the other hand, due to their cantilever type of kinematicarrangement, fully serial manipulators suffer from a lack of stiffness and fromrelatively large positioning errors. The hybrid manipulator studied isintrinsically stiffer and more accurate. Furthermore, since all actuators arelocated on the first axis, the inertial effects are considerably reduced. Inaddition, it is shown that the special kinematic structure of our manipulatorhas the potential of avoiding parallel singularities by a suitable choice ofthe \"working mode\", thus leading to larger workspaces. The influence of thedifferent structural dimensions (e.g. the link lengths) on the kinematic andmechanical properties are analysed in view of the optimal design of such hybridmanipulators.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "In 1929 Heisenberg and Pauli laid the foundations of QFT by quantizing thefields (method of canonical quantization). This general theory of quantizedfields has remained undisputed up to now. We show how the unmodifiedHeisenberg-Pauli calculations make sense mathematically by using a theory ofgeneralized functions adapted to nonlinear operations. By providing anappropriate mathematical setting, nonlinear generalized functions open doorsfor their understanding but there remains presumably very hard technicalproblems. (i) Domains of the interacting field operators: a priori the H-Pcalculations give time dependent dense domains, what is not very convenient;(ii) Calculations of the resulting matrix elements of the S operator: from theunitarity of the S operator as a whole there are no longer ``infinities,'' buta priori there is no other hope than heavy computer calculations; (iii)Connection with renormalization theory: it should provide an approximation whenthe coupling constant is small. The aim of this paper is to present, on thegrounds of a standard mathematical model of QFT (a self interacting scalarboson field), a basis for improvement without significant prerequisites inmathematics and physics. It is an attempt to use nonlinear generalizedfunctions in QFT, starting directly from the calculations made by physicists,in the same way as they have already been used in classical mechanics andgeneral relativity.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "In this paper, the notion of {\\em $p$-adic multiresolution analysis (MRA)} isintroduced. We use a ``natural'' refinement equation whose solution (arefinable function) is the characteristic function of the unit disc. Thisequation reflects the fact that the characteristic function of the unit disc isthe sum of $p$ characteristic functions of disjoint discs of radius $p^{-1}$.The case $p=2$ is studied in detail. Our MRA is a 2-adic analog of the realHaar MRA. But in contrast to the real setting, the refinable functiongenerating our Haar MRA is periodic with period 1, which never holds for realrefinable functions. This fact implies that there exist infinity many different2-adic orthonormal wavelet bases in ${\\cL}^2(\\bQ_2)$ generated by the same HaarMRA. All of these bases are constructed. Since $p$-adic pseudo-differentialoperators are closely related to wavelet-type bases, our bases can beintensively used for applications.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "A rotating bosonic many-body system in a harmonic trap is studied with the3D-Cranked Hartree-Fock-Bogoliubov method at zero temperature, which has beenapplied to nuclear many-body systems at high spin. This method is a variationalmethod extended from the Hartree-Fock theory, which can treat the pairingcorrelations in a self-consistent manner. An advantage of this method is that afinite-range interaction between constituent particles can be used in thecalculation, unlike the original Gross-Pitaevskii approach. To demonstrate thevalidity of our method, we present a calculation for a toy model, that is, arotating system of ten bosonic particles interacting through the repulsivequadrupole-quadrupole interaction in a harmonic trap. It is found that theyrast states, the lowest-energy states for the given total angular momentum,does not correspond to the Bose-Einstein condensate, except a few specialcases. One of such cases is a vortex state, which appears when the totalangular momentum $L$ is twice the particle number $N$ (i.e., $L=2N$).", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Through polarization observations masers are unique probes of the magneticfield in a variety of different astronomical objects, with the different maserspecies tracing different physical conditions. In recent years maserpolarization observations have provided insights in the magnetic field strengthand morphology in, among others, the envelopes around evolved stars, PlanetaryNebulae (PNe), massive star forming regions and supernova remnants. Morerecently, maser observations have even been used to determine the magneticfield in megamaser galaxies. This review will present an overview of maserpolarization observations and magnetic field determinations of the last severalyears and discuss the implications of the magnetic field measurements forseveral important fields of study, such as aspherical PNe creation and massivestar formation.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The existence of neutrino masses strongly suggests that right-handedneutrinos exist, but the data do not favor any particular scale for theMajorana mass parameters. Here I explore the possibility that these particlesexist at the electroweak scale along with additional new physics at the TeVscale . Higher dimension operators involving right-handed neutrinos and theHiggs boson can introduce new decay modes of the Higgs boson, significantlymodifying its phenomenology if it is light. With minimal flavor violation theHiggs boson cascade decays to 6 particles containing two highly displacedvertices. Each displaced vertex produces an odd number of leptons, leading to adramatic signature of overall lepton violation at each vertex. I discuss thelimits from the Tevatron, and find that they are close to exploring interestingregions of parameters, while limiting others. Moving beyond minimal flavorviolation, cascade decays of the Higgs boson into as many as 14 particles canoccur.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Surface roughness becomes relevant if typical length scales of the system arecomparable to the scale of the variations as it is the case in microfluidicsetups. Here, an apparent boundary slip is often detected which can have itsorigin in the assumption of perfectly smooth boundaries. We investigate theproblem by means of lattice Boltzmann (LB) simulations and introduce an``effective no-slip plane'' at an intermediate position between peaks andvalleys of the surface. Our simulations show good agreement with analyticalresults for sinusoidal boundaries, but can be extended to arbitrary geometriesand experimentally obtained surface data. We find that the detected apparentslip is independent of the detailed boundary shape, but only given by thedistribution of surface heights. Further, we show that the slip diverges as theamplitude of the roughness increases.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We show that hard-scattering factorization is violated in the production ofhigh-p_T hadrons in hadron-hadron collisions, in the case that the hadrons areback-to-back, so that k_T factorization is to be used. The explicitcounterexample that we construct is for the single-spin asymmetry with one beamtransversely polarized. The Sivers function needed here has particularsensitivity to the Wilson lines in the parton densities. We use a greatlysimplified model theory to make the breakdown of factorization easy to checkexplicitly. But the counterexample implies that standard arguments forfactorization fail not just for the single-spin asymmetry but for theunpolarized cross section for back-to-back hadron production in QCD inhadron-hadron collisions. This is unlike corresponding cases in e^+e^-annihilation, Drell-Yan, and deeply inelastic scattering. Moreover, the resultendangers factorization for more general hadroproduction processes.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We study the dc conductance of organic single-molecule contacts in thepresence of external electromagnetic radiation (photoconductance). In agreementwith previous predictions, we find that the radiation can lead to largeenhancements of the conductance of such contacts by bringing off-resonantlevels into resonance through photoassisted processes. In our analysis we makeuse of the simplifying fact that, under certain assumptions, thephotoconductance can be expressed in terms of the transmission function in theabsence of the radiation. The conductance enhancement is demonstrated foroligophenylene molecules between gold electrodes, whose electronic structure iscalculated based on density-functional theory. It is shown that the exponentialdecay of the conductance with the length of the molecule can be replaced by alength-independent value in the presence of radiation.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "As the dimensionality is reduced, the world becomes more and moreinteresting; novel and fascinating phenomena show up which call forunderstanding. Physics in one dimension is a fascinating topic for theory andexperiment: for the former often a simplification, for the latter always achallenge. Various ways will be demonstrated how one-dimensional structures canbe achieved in reality. In particular organic conductors could establishthemselves as model systems for the investigation of the physics in reduceddimensions.  In the metallic state of a one-dimensional solid, Fermi-liquid theory breaksdown and spin and charge degrees of freedom become separated. But the metallicphase is not stable in one dimension: as the temperature is reduced, theelectronic charge and spin tend to arrange themselves in an ordered fashion dueto strong correlations. The competition of the different interactions isresponsible for which broken-symmetry ground state is eventually realized in aspecific compound and which drives the system towards an insulating state.  Here we review the various ordering phenomena and how they can be identifiedby dielectric and optic measurements.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "In the framework of the model inter-comparison study - Asia Phase II (MICS2),where eight models are compared over East Asia, this paper studies theinfluence of different parameterizations used in the aerosol module on theaerosol concentrations of sulfate and nitrate in PM10. An intracomparison ofaerosol concentrations is done for March 2001 using different configurations ofthe aerosol module of one of the model used for the intercomparison. Singlemodifications of a reference setup for model configurations are performed andcompared to a reference case. These modifications concern the sizedistribution, i.e. the number of sections, and physical processes, i.e.coagulation, condensation/evaporation, cloud chemistry, heterogeneous reactionsand sea-salt emissions. Comparing monthly averaged concentrations at differentstations, the importance of each parameterization is first assessed. It isfound that sulfate concentrations are little sensitive to sea-salt emissionsand to whether condensation is computed dynamically or by assumingthermodynamic equilibrium. Nitrate concentrations are little sensitive to cloudchemistry. However, a very high sensitivity to heterogeneous reactions isobserved. Thereafter, the variability of the aerosol concentrations to the useof different chemistry transport models (CTMs) and the variability to the useof different parameterizations in the aerosol module are compared. For sulfate,the variability to the use of different parameterizations in the aerosol moduleis lower than the variability to the use of different CTMs. However, fornitrate, for monthly averaged concentrations averaged over four stations, thesetwo variabilities have the same order of magnitude.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "This paper introduces a continuous model for Multi-cellular DevelopmentalDesign. The cells are fixed on a 2D grid and exchange \"chemicals\" with theirneighbors during the growth process. The quantity of chemicals that a cellproduces, as well as the differentiation value of the cell in the phenotype,are controlled by a Neural Network (the genotype) that takes as inputs thechemicals produced by the neighboring cells at the previous time step. In theproposed model, the number of iterations of the growth process is notpre-determined, but emerges during evolution: only organisms for which thegrowth process stabilizes give a phenotype (the stable state), others aredeclared nonviable. The optimization of the controller is done using the NEATalgorithm, that optimizes both the topology and the weights of the NeuralNetworks. Though each cell only receives local information from its neighbors,the experimental results of the proposed approach on the 'flags' problems (thephenotype must match a given 2D pattern) are almost as good as those of adirect regression approach using the same model with global information.Moreover, the resulting multi-cellular organisms exhibit almost perfectself-healing characteristics.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Cold dark matter haloes are populated by caustics, which are yet to beresolved in N-body simulations or observed in the Universe. Secondary infallmodel provides a paradigm for the study of caustics in \"typical\" haloesassuming that they have had no major mergers and have grown only by smoothaccretion. This is a particular characteristic of the smallest dark matterhaloes of about 10^{-5} Mo, which although \"atypical\" contain no substructuresand could have survived until now with no major mergers. Thus using this modelas the first guidline, we evaluate the neutralino self-annihilation flux forthese haloes. Our results show that caustics could leave a distinct sawteethsignature on the differential and cumulative fluxes coming from the outerregions of these haloes. The total annihilation signal from the regions awayfrom the centre can be boosted by about forty percents.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "A long standing problem is the supergauge completion of AdS_4 x (G/H)_7 orAdS_5 x (G/H)_5 backgrounds which preserve less then maximal supersymmetry. Inparallel with the supersolvable realization of the AdS_4 x S^7 background basedon Kappa-symmetry, we develop a technique which amounts to solving theabove-mentioned problem in a way useful for pure spinor quantization forsupermembranes and superstrings. Instead of gauge fixing some of the superspacecoordinates to zero, we impose an additional constraint on them reproducing thesimplifications of the supersolvable representations. The constraints arequadratic, homogeneous, Sp(4,R)-covariant, and consistent from the quantumpoint of view in the pure spinor approach. Here we provide the geometricalsolution which, in a subsequent work, will be applied to the membrane and thesuperstring sigma models.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present spectroscopic observations of 11 moderately high-redshift (z~0.7-1.0) clusters from the first Red-Sequence Cluster Survey (RCS-1). We findexcellent agreement between the red-sequence estimated redshift and thespectroscopic redshift, with a scatter of 10% at z>0.7. At the high-redshiftend (z>~0.9) of the sample, we find two of the systems selected are projectionsof pairs of comparably rich systems, with red-sequences too close todiscriminate in (R-z') colour. In one of these systems, the two components areclose enough to be physically associated. For a subsample of clusters withsufficient spectroscopic members, we examine the correlation between B_gcR(optical richness) and the dynamical mass inferred from the velocitydispersion. We find these measurements to be compatible, within the relativelylarge uncertainties, with the correlation established at lower redshift for theX-ray selected CNOC1 clusters and also for a lower redshift sample of RCS-1clusters. Confirmation of this and calibration of the scatter in the relationwill require larger samples of clusters at these and higher redshifts.[abridged]", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "[Abridged] We test the accuracy of different models of the attenuation oflight due to resonant scattering by intergalactic neutral hydrogen by comparingtheir predictions of the evolution of the mean cosmic flux decrement, D_A, tomeasurements of this quantity based on observations. To this end, we use dataavailable in the literature and our own measurements of the cosmic fluxdecrement for 25 quasars in the redshift range 2.71 < z < 5.41 taken from theSDSS Data Release 5. In order to perform the measurements of D_A, we fit apower-law to the continuum redward of the Lya emission line, and extrapolatethis fit to region blueward of it, where the flux is severely affected byabsorption due to intervening HI absorbers. We compute, using numericalsimulations, the redshift evolution of D_A accounting for the presence of LyaForest absorbers and Lyman limit systems randomly distributed along theline-of-sight, and compute its intrinsic scatter at the 1-, 2-, and 3-sigmalevel due to fluctuations in the absorber properties (column density, Dopplerparameter, redshift) along different lines-of-sight. The numerical simulationsconsist of Monte Carlo realizations of distributions of the absorber propertiesconstrained from observations. The results from the models considered hereconfirm our theoretical expectation that the distribution of D_A at any givenredshift be well described by a lognormal distribution function. This impliesthat the effective optical depth, usually defined as the negative logarithm ofthe average flux, 1 - D_A, is very accurately Gaussian distributed, in contrastto previous studies. This result is independent to the form of the inputdistribution functions, and rather insensitive to the presence of high-columndensity absorbers, such as the Lyman limit systems.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The bipolar HH 212 outflow has been mapped in SiO using the extendedconfiguration of the Plateau de Bure Interferometer (PdBI), revealing a highlycollimated SiO jet closely associated with the H2 jet component. We study atunprecedented resolution (0.34\" across the jet axis) the properties of theinnermost SiO ``microjet'' within 1000 AU of this young Class 0 source, tocompare it with atomic microjets from more evolved sources and to constrain itsorigin. The SiO channel maps are used to investigate the microjet collimationand velocity structure. A large velocity gradient analysis is applied to SiO(2-1), (5-4) and (8-7) data from the PdBI and the Submillimeter Array toconstrain the SiO opacity and abundance. The HH212 Class 0 microjet showsstriking similarities in collimation and energetic budget with atomic microjetsfrom T Tauri sources. Furthermore, the SiO lines appear optically thick, unlikewhat is generally assumed. We infer T(kin) ~ 50-500 K and an SiO/H2 abundancegreater than 4 10(-8)-6 10(-5) for n(H2) = 10(7)-10(5) cm(-3), i.e. 0.05-90% ofthe elemental silicon. This similar jet width, regardless of the presence of adense envelope, definitely rules out jet collimation by external pressure, andfavors a common MHD self-collimation (and possibly acceleration) process at allstages of star formation. We propose that the more abundant SiO in Class 0 jetscould mainly result from rapid (less than 25 yrs) molecular synthesis at highjet densities.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The temperature variation effect of shape anisotropy on the coercivity,HC(T), for the aligned Stoner-Wohlfarth (SW) soft ferromagnets, such as fcc Ni,fcc Co and bcc Fe, are investigated within the framework of Neel-Brown (N-B)analysis. An extended N-B equation is thus proposed,by introducing a singledimensionless correction function, the reduced magnetization, m(\\tao) =MS(T)/MS(0), in which \\tao = T/TC is the reduced temperature, MS(T) is thesaturation magnetization, and TC is the Curie temperature. The factor, m(\\tao),accounts for the temperature-dependent effect of the shape anisotropy. Theconstants, H0 and E0, are for the switching field at zero temperature and thepotential barrier at zero field, respectively. According to this newly derivedequation, the blocking temperature above which the properties ofsuperparamagnetism show up is described by the expression, TB =E0m^2(\\tao)/[kBln(t/t0)], with the extra correction factor m^2(\\tao). Thepossible effect on HC(T) and the blocking temperature, TB, attributed to thedownshift of TC resulting from the finite size effect has been discussed also.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present an analysis of the Lyman alpha forests of five quasar spectra inthe near UV. Properties of the intergalactic medium (IGM) at an intermediateredshift interval (0.9 < z < 1.9) are studied. The amount of baryons in thediffuse photoionised IGM and the warm-hot intergalactic medium (WHIM) aretraced to get constraints on the redshift evolution of the different phases ofthe intergalactic gas. The baryon density of the diffuse IGM is determined withphotoionisation calculations under the assumption of local hydrostaticequilibrium. We assume that the gas is ionised by a metagalactic backgroundradiation with a Haardt & Madau (2001) spectrum. The WHIM is traced with broadLyman alpha (BLA) absorption. The properties of a number of BLA detections arestudied. Under the assumption of collisional ionisation equilibrium a lowerlimit to the baryon density could be estimated. It is found that the diffusephotoionised IGM contains at least 25% of the total baryonic matter atredshifts 1 < z < 2. For the WHIM a lower limit of 2.4% could be determined.Furthermore the data indicates that the intergalactic gas is in a state ofevolution at z=1.5. We confirm that a considerable part of the WHIM is createdbetween z=1 and z=2.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Consider the partition function of a directed polymer in an IID field. Weassume that both tails of the negative and the positive part of the field areat least as light as exponential. It is a well-known fact that the free energyof the polymer is equal to a deterministic constant for almost everyrealization of the field and that the upper tail of the large deviations isexponential. The lower tail of the large deviations is typically lighter thanexponential. In this paper we provide a method to obtain estimates on the rateof decay of the lower tail of the large deviations, which are sharp up tomultiplicative constants. As a consequence, we show that the lower tail of thelarge deviations exhibits three regimes, determined according to the tail ofthe negative part of the field. Our method is simple to apply and can be usedto cover other oriented and non-oriented models including first/last-passagepercolation and the parabolic Anderson model", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Utilizing an eigenfunction decomposition, we study the growth and spectra ofenergy in the vortical and wave modes of a 3D rotating stratified fluid as afunction of $\\epsilon = f/N$. Working in regimes characterized by moderateBurger numbers, i.e. $Bu = 1/\\epsilon^2 < 1$ or $Bu \\ge 1$, our resultsindicate profound change in the character of vortical and wave modeinteractions with respect to $Bu = 1$. As with the reference state of$\\epsilon=1$, for $\\epsilon < 1$ the wave mode energy saturates quite quicklyand the ensuing forward cascade continues to act as an efficient means ofdissipating ageostrophic energy. Further, these saturated spectra steepen as$\\epsilon$ decreases: we see a shift from $k^{-1}$ to $k^{-5/3}$ scaling for$k_f < k < k_d$ (where $k_f$ and $k_d$ are the forcing and dissipation scales,respectively). On the other hand, when $\\epsilon > 1$ the wave mode energynever saturates and comes to dominate the total energy in the system. In fact,in a sense the wave modes behave in an asymmetric manner about $\\epsilon = 1$.With regard to the vortical modes, for $\\epsilon \\le 1$, the signatures of 3Dquasigeostrophy are clearly evident. Specifically, we see a $k^{-3}$ scalingfor $k_f < k < k_d$ and, in accord with an inverse transfer of energy, thevortical mode energy never saturates but rather increases for all $k < k_f$. Incontrast, for $\\epsilon > 1$ and increasing, the vortical modes contain aprogressively smaller fraction of the total energy indicating that the 3Dquasigeostrophic subsystem plays an energetically smaller role in the overalldynamics.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "A series of semi-inclusive deep-inelastic scattering measurements ondeuterium, helium, neon, krypton, and xenon targets has been performed in orderto study hadronization. The data were collected with the HERMES detector at theDESY laboratory using a 27.6 GeV positron or electron beam. Hadronmultiplicities on nucleus A relative to those on the deuteron, R_A^h, arepresented for various hadrons (\\pi^+, \\pi^-, \\pi^0, K^+, K^-, p, and \\bar{p})as a function of the virtual-photon energy \\nu, the fraction z of this energytransferred to the hadron, the photon virtuality Q^2, and the hadron transversemomentum squared p_t^2. The data reveal a systematic decrease of R_A^h with themass number A for each hadron type h. Furthermore, R_A^h increases (decreases)with increasing values of \\nu (z), increases slightly with increasing Q^2, andis almost independent of p_t^2, except at large values of p_t^2. For pionstwo-dimensional distributions also are presented. These indicate that thedependences of R_A^{\\pi} on \\nu and z can largely be described as a dependenceon a single variable L_c, which is a combination of \\nu and z. The dependenceon L_c suggests in which kinematic conditions partonic and hadronic mechanismsmay be dominant. The behaviour of R_A^{\\pi} at large p_t^2 constitutestentative evidence for a partonic energy-loss mechanism. The A-dependence ofR_A^h is investigated as a function of \\nu, z, and of L_c. It approximatelyfollows an A^{\\alpha} form with \\alpha \\approx 0.5 - 0.6.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "High dispersion near-infrared spectra have been taken of sevenhighly-evolved, variable, intermediate-mass (4-6 Msun) AGB stars in the LMC andSMC in order to look for C, N and O variations that are expected to arise fromthird dredge-up and hot-bottom burning. The pulsation of the objects has beenmodelled, yielding stellar masses, and spectral synthesis calculations havebeen performed in order to derive abundances from the observed spectra. For twostars, abundances of C, N, O, Na, Al, Ti, Sc and Fe were derived and comparedwith the abundances predicted by detailed AGB models. Both stars show verylarge N enhancements and C deficiencies. These results provide the firstobservational confirmation of the long-predicted production of primary nitrogenby the combination of third dredge-up and hot-bottom burning inintermediate-mass AGB stars. It was not possible to derive abundances for theremaining five stars: three were too cool to model, while another two hadstrong shocks in their atmospheres which caused strong emission to fill theline cores and made abundance determination impossible. The latter occurrenceallows us to predict the pulsation phase interval during which observationsshould be made if successful abundance analysis is to be possible.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "In the previous study (Hiremath 2006a), the solar cycle is modeled as aforced and damped harmonic oscillator and from all the 22 cycles (1755-1996),long-term amplitudes, frequencies, phases and decay factor are obtained. Usingthese physical parameters of the previous 22 solar cycles and by an {\\emautoregressive model}, we predict the amplitude and period of the futurefifteen solar cycles. Predicted amplitude of the present solar cycle (23)matches very well with the observations. The period of the present cycle isfound to be 11.73 years. With these encouraging results, we also predict theprofiles of future 15 solar cycles. Important predictions are : (i) the periodand amplitude of the cycle 24 are 9.34 years and 110 ($\\pm 11$), (ii) theperiod and amplitude of the cycle 25 are 12.49 years and 110 ($\\pm$ 11), (iii)during the cycles 26 (2030-2042 AD), 27 (2042-2054 AD), 34 (2118-2127 AD), 37(2152-2163 AD) and 38 (2163-2176 AD), the sun might experience a very highsunspot activity, (iv) the sun might also experience a very low (around 60)sunspot activity during cycle 31 (2089-2100 AD) and, (v) length of the solarcycles vary from 8.65 yrs for the cycle 33 to maximum of 13.07 yrs for thecycle 35.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "This paper presents a geometric description of Lagrangian and Hamiltoniansystems on Lie affgebroids subject to affine nonholonomic constraints. Wedefine the notion of nonholonomically constrained system, and characterizeregularity conditions that guarantee that the dynamics of the system can beobtained as a suitable projection of the unconstrained dynamics. It is shownthat one can define an almost aff-Poisson bracket on the constraint AV-bundle,which plays a prominent role in the description of nonholonomic dynamics.Moreover, these developments give a general description of nonholonomic systemsand the unified treatment permits to study nonholonomic systems after or beforereduction in the same framework. Also, it is not necessary to distinguishbetween linear or affine constraints and the methods are valid for explicitlytime-dependent systems.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We consider the accretion process in a disk with magnetic fields that aredragged in from the interstellar medium by gravitational collapse. Twodiffusive processes are at work in the system: (1) \"viscous\" torques exerted byturbulent and magnetic stresses, and (2) \"resistive\" redistribution of masswith respect to the magnetic flux arising from the imperfect conduction ofcurrent. In steady state, self-consistency between the two rates of driftrequires that a relationship exists between the coefficients of turbulentviscosity and turbulent resistivity. Ignoring any interactions with a stellarmagnetosphere, we solve the steady-state equations for a magnetized disk underthe gravitational attraction of a mass point and threaded by an amount ofmagnetic flux consistent with calculations of magnetized gravitational collapsein star formation. Our model mean-field equations have an exact analyticalsolution that corresponds to magnetically diluted Keplerian rotation about thecentral mass point. The solution yields the strength of the magnetic field andthe surface density as functions of radial position in the disk and theirconnection with the departure from pure Keplerian rotation in representativecases. We compare the predictions of the theory with the available observationsconcerning T Tauri stars, FU Orionis stars, and low- and high-mass protostars.Finally, we speculate on the physical causes for high and low states of theaccretion disks that surround young stellar objects. One of the more importantresults of this study is the physical derivation of analytic expressions forthe turbulent viscosity and turbulent resistivity.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "When the DNA double helix is subjected to external forces it can stretchelastically to elongations reaching 100% of its natural length. Thesedistortions, imposed at the mesoscopic or macroscopic scales, have a dramaticeffect on electronic properties at the atomic scale and on electrical transportalong DNA. Accordingly, a multiscale approach is necessary to capture theelectronic behavior of the stretched DNA helix. To construct such a model, webegin with accurate density-functional-theory calculations for electronicstates in DNA bases and base pairs in various relative configurationsencountered in the equilibrium and stretched forms. These results arecomplemented by semi-empirical quantum mechanical calculations for the statesof a small size [18 base pair poly(CG)-poly(CG)] dry, neutral DNA sequence,using previously published models for stretched DNA. The calculated electronicstates are then used to parametrize an effective tight-binding model that candescribe electron hopping in the presence of environmental effects, such as thepresence of stray water molecules on the backbone or structural features of thesubstrate. These effects introduce disorder in the model hamiltonian whichleads to electron localization. The localization length is smaller by severalorders of magnitude in stretched DNA relative to that in the unstretchedstructure.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "OH 231.8+4.2 is a well studied preplanetary nebula (pPN) around a binarystellar system that shows a remarkable bipolar outflow. To study the structureand kinematics of the inner 10-80 AU nebular regions we performedhigh-resolution observations of the H$_2$O 6$_{1,6}$--5$_{2,3}$ and $^{28}$SiO$v$=2, $J$=1--0 maser emissions with the Very Long Baseline Array. The absoluteposition of both emission distributions were recovered using the phasereferencing technique, and accurately registered in HST optical images. H$_2$Omaser clumps are found to be distributed in two areas of 20 mas in sizespatially displaced by $\\sim$60 milli-arcseconds along an axis oriented nearlynorth-south. SiO masers are tentatively found to be placed between the twoH$_2$O maser emitting regions, probably indicating the position of the Miracomponent of the system. The SiO maser emission traces an inner equatorialcomponent with a diameter of 12 AU, probably a disk rotating around the M-typestar. Outwards, we detect in the H$_2$O data a pair of polar caps, separated by80 AU. We believe that the inner regions of the nebula probably have beenaltered by the presence of the companion, leading to an equator-to-pole densitycontrast that may explain the lack of H$_2$O masers and strong SiO maseremission in the denser, equatorial regions.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Population structure induced by both spatial embedding and more generalnetworks of interaction, such as model social networks, have been shown to havea fundamental effect on the dynamics and outcome of evolutionary games. Theseeffects have, however, proved to be sensitive to the details of the underlyingtopology and dynamics. Here we introduce a minimal population structure that isdescribed by two distinct hierarchical levels of interaction. We believe thismodel is able to identify effects of spatial structure that do not depend onthe details of the topology. We derive the dynamics governing the evolution ofa system starting from fundamental individual level stochastic processesthrough two successive meanfield approximations. In our model of populationstructure the topology of interactions is described by only two parameters: theeffective population size at the local scale and the relative strength of localdynamics to global mixing. We demonstrate, for example, the existence of acontinuous transition leading to the dominance of cooperation in populationswith hierarchical levels of unstructured mixing as the benefit to cost ratiobecomes smaller then the local population size. Applying our model of spatialstructure to the repeated prisoner's dilemma we uncover a novel andcounterintuitive mechanism by which the constant influx of defectors sustainscooperation. Further exploring the phase space of the repeated prisoner'sdilemma and also of the \"rock-paper-scissor\" game we find indications of richstructure and are able to reproduce several effects observed in other modelswith explicit spatial embedding, such as the maintenance of biodiversity andthe emergence of global oscillations.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Epitaxial self-assembled quantum dots (SAQDs) are of interest fornanostructured optoelectronic and electronic devices such as lasers,photodetectors and nanoscale logic. Spatial order and size order of SAQDs areimportant to the development of usable devices. It is likely that these twotypes of order are strongly linked; thus, a study of spatial order will alsohave strong implications for size order. Here a study of spatial order isundertaken using a linear analysis of a commonly used model of SAQD formationbased on surface diffusion. Analytic formulas for film-height correlationfunctions are found that characterize quantum dot spatial order andcorresponding correlation lengths that quantify order. Initial atomic-scalerandom fluctuations result in relatively small correlation lengths (about twodots) when the effect of a wetting potential is negligible; however, thecorrelation lengths diverge when SAQDs are allowed to form at a near-criticalfilm height. The present work reinforces previous findings about anisotropy andSAQD order and presents as explicit and transparent mechanism for ordering withcorresponding analytic equations. In addition, SAQD formation is by its naturea stochastic process, and various mathematical aspects regarding statisticalanalysis of SAQD formation and order are presented.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Sub-100 nm nanomagnets not only are technologically important, but alsoexhibit complex magnetization reversal behaviors as their dimensions arecomparable to typical magnetic domain wall widths. Here we capture magnetic\"fingerprints\" of 1 billion Fe nanodots as they undergo a single domain tovortex state transition, using a first-order reversal curve (FORC) method. Asthe nanodot size increases from 52 nm to 67 nm, the FORC diagrams revealstriking differences, despite only subtle changes in their major hysteresisloops. The 52 nm nanodots exhibit single domain behavior and the coercivitydistribution extracted from the FORC distribution agrees well with acalculation based on the measured nanodot size distribution. The 58 and 67 nmnanodots exhibit vortex states, where the nucleation and annihilation of thevortices are manifested as butterfly-like features in the FORC distribution andconfirmed by micromagnetic simulations. Furthermore, the FORC method givesquantitative measures of the magnetic phase fractions, and vortex nucleationand annihilation fields.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We investigate the accuracy of astrometric measurements with the VLT/FORS1camera and consider potential applications. The study is based on two-epoch(2000 and 2002/2003) frame series of observations of a selected Galactic Bulgesky region that were obtained with FORS1 during four consecutive nights each.Reductions were carried out with a novel technique that eliminates atmosphericimage motion and does not require a distinction between targets and referenceobjects. The positional astrometric precision was found to be limited only bythe accuracy of the determination of the star photocentre, which is typically200-300 microarcsec per single measurement for bright unsaturated starsB=18-19. Several statistical tests have shown that at time-scales of 1-4 nightsthe residual noise in measured positions is essentially a white noise with nosystematic instrumental signature and no significant deviation from a Gaussiandistribution. Some evidence of a good astrometric quality of the VLT for framesseparated by two years has also been found. Our data show that the VLT withFORS1/2 cameras can be effectively used for astrometric observations ofplanetary microlensing events and other applications where a high accuracy isrequired, that is expected to reach 30-40 microarcsec for a series of 50 frames(one hours with R filter).", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The purpose of the present work is to treat a new notion related to lineardynamics, which can be viewed as a \"localization\" of the notion ofhypercyclicity. In particular, let $T$ be a bounded linear operator acting on aBanach space $X$ and let $x$ be a non-zero vector in $X$ such that for everyopen neighborhood $U\\subset X$ of $x$ and every non-empty open set $V\\subset X$there exists a positive integer $n$ such that $T^{n}U\\cap V\\neq\\emptyset$. Inthis case $T$ will be called a $J$-class operator. We investigate the class ofoperators satisfying the above property and provide various examples. It isworthwhile to mention that many results from the theory of hypercyclicoperators have their analogues in this setting. For example we establishresults related to the Bourdon-Feldman theorem and we characterize the$J$-class weighted shifts. We would also like to stress that even non-separableBanach spaces which do not support topologically transitive operators, as forexample $l^{\\infty}(\\mathbb{N})$, do admit $J$-class operators.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "WIMPs with electroweak scale masses (neutralinos, etc.) remain in kineticequilibrium with other particle species until temperatures approximately in therange of 10 MeV to 1 GeV, leading to the formation of dark matter substructurewith masses as small as $10^{-4} M_{\\odot}$ to $10^{-12} M_{\\odot}$. However,if dark matter consists of particles with MeV scale masses, as motivated by theobservation of 511 keV emission from the Galactic Bulge, such particles arenaturally expected to remain in kinetic equilibrium with the cosmic neutrinobackground until considerably later times. This would lead to a strongsuppression of small scale structure with masses below about $10^7 M_{\\odot}$to $10^4 M_{\\odot}$. This cutoff scale has important implications for presentand future searches for faint Local Group satellite galaxies and for themissing satellites problem.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The origin of the ultrahigh-energy (UHE) cosmic rays (CRs) from the secondknee ($\\sim6\\times10^{17}$eV) above in the CR spectrum is still unknown.Recently, there has been growing evidence that a peculiar type of supernovae,called hypernovae, are associated with sub-energetic gamma-ray bursts (GRBs),such as SN1998bw/GRB980425 and SN2003lw/GRB031203. Such hypernovae appear tohave high (up to mildly relativistic) velocity ejecta, which may be linked tothe sub-energetic GRBs. Assuming a continuous distribution of the kineticenergy of the hypernova ejecta as a function of its velocity $E_k\\propto(\\Gamma\\beta)^{-\\alpha}$ with $\\alpha\\sim 2$, we find that 1) the externalshock wave produced by the high velocity ejecta of a hypernova can accelerateprotons up to energies as high as $10^{19} {\\rm eV}$; 2) the cosmologicalhypernova rate is sufficient to account for the energy flux above the secondknee; and 3) the steeper spectrum of CRs at these energies can arise in thesesources. In addition, hypernovae would also give rise to a faint diffuse UHEneutrino flux, due to $p\\gamma$ interactions of the UHE CRs with hypernovaoptical-UV photons.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We consider gradient fields $(\\phi_x:x\\in \\mathbb{Z}^d)$ whose law takes theGibbs--Boltzmann form $Z^{-1}\\exp\\{-\\sum_{< x,y>}V(\\phi_y-\\phi_x)\\}$, where thesum runs over nearest neighbors. We assume that the potential $V$ admits therepresentation \\[V(\\eta):=-\\log\\int\\varrho({d}\\kappa)\\exp\\biggl[-{1/2}\\kappa\\eta^2\\biggr],\\] where $\\varrho$ is a positive measure with compact support in$(0,\\infty)$. Hence, the potential $V$ is symmetric, but nonconvex in general.While for strictly convex $V$'s, the translation-invariant, ergodic gradientGibbs measures are completely characterized by their tilt, a nonconvexpotential as above may lead to several ergodic gradient Gibbs measures withzero tilt. Still, every ergodic, zero-tilt gradient Gibbs measure for thepotential $V$ above scales to a Gaussian free field.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "This paper focuses on the issue of energy efficiency in wireless datanetworks through a game theoretic approach. The case considered is that inwhich each user is allowed to vary its transmit power, spreading code, anduplink receiver in order to maximize its own utility, which is here defined asthe ratio of data throughput to transmit power. In particular, the case inwhich linear multiuser detectors are employed at the receiver is treated first,and, then, the more challenging case in which non-linear decision feedbackmultiuser receivers are adopted is addressed. It is shown that, for bothreceivers, the problem at hand of utility maximization can be regarded as anon-cooperative game, and it is proved that a unique Nash equilibrium pointexists. Simulation results show that significant performance gains can beobtained through both non-linear processing and spreading code optimization; inparticular, for systems with a number of users not larger than the processinggain, remarkable gains come from spreading code optimization, while, foroverloaded systems, the largest gainscome from the use of non-linearprocessing. In every case, however, the non-cooperative games proposed here areshown to outperform competing alternatives.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Apart from its mass and width, the most important property of a new chargedgauge boson, $W'$, is the helicity of its couplings to the SM fermions. Suchparticles are expected to exist in many extensions of the Standard Model. Inthis paper we explore the capability of the LHC to determine the $W'$ couplinghelicity at low integrated luminosities in the $\\ell +E_T^{miss}$ discoverychannel. We find that measurements of the transverse mass distribution,reconstructed from this final state in the $W-W'$ interference region, providesthe best determination of this quantity. To make such measurements requiresintegrated luminosities of $\\sim 10(60) fb^{-1}$ assuming $M_{W'}=1.5(2.5)$ TeVand provided that the $W'$ couplings have Standard Model magnitude. Thishelicity determination can be further strengthened by the use of variousdiscovery channel leptonic asymmetries, also measured in the same interferenceregime, but with higher integrated luminosities.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Let $(M,g,\\si)$ be a compact spin manifold of dimension $n \\geq 2$. Let$\\lambda_1^+(\\tilde{g})$ be the smallest positive eigenvalue of the Diracoperator in the metric $\\tilde{g} \\in [g]$ conformal to $g$. We then define$\\lamin(M,[g],\\si) = \\inf_{\\tilde{g} \\in [g]} \\lambda_1^+(\\tilde{g})\\Vol(M,\\tilde{g})^{1/n} $. We show that $0< \\lamin(M,[g],\\si) \\leq\\lamin(\\mS^n)$. %=\\frac{n}{2} \\om_n^{{1 \\over n}}$ . We find sufficientconditions for which we obtain strict inequality $\\lamin(M,[g],\\si) <\\lamin(\\mS^n)$. This strict inequality has applications to conformal spingeometry.  -----  Soit $(M,g,\\si)$ une vari\\'et\\'e spinorielle compacte de dimension $n \\geq2$. %Si $\\tilde{g} \\in [g]$ est une m\\'etrique conforme \\`a $g$, On note$\\lambda_1^+(\\tilde{g})$ la plus petite valeur propre $>0$ de l'op\\'erateur deDirac dans la m\\'etrique $\\tilde{g} \\in [g]$ conforme \\`a $g$. On d\\'efinit$\\lamin(M,[g],\\si) = \\inf_{\\tilde{g} \\in [g]} \\lambda_1^+(\\tilde{g})  \\Vol(M,\\tilde{g})^{1/n} $. On montre que $0< \\lamin(M,[g],\\si) \\leq\\lamin(\\mS^n)$. %= \\frac{n}{2} \\om_n^{{1 \\over n}}$ On trouve des conditionssuffisantes pour lesquelles on obtient l'in\\'egalit\\'e stricte$\\lamin(M,[g],\\si) < \\lamin(\\mS^n)$. Cette in\\'egalit\\'e stricte a desapplications en g\\'eom\\'etrie spinorielle conforme.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "A path-integral for the t-J model in two dimensions is constructed based onDirac quantization, with an action found originally by Wiegmann (Phys. Rev.Lett. {\\bf 60}, 821 (1988); Nucl. Phys. B323, 311 (1989)). Concentrating on thelow doping limit, we assume short range antiferromagnetic order of the spindegrees of freedom. Going over to a local spin quantization axis of the dopantfermions, that follows the spin degree of freedom, staggered CP$^1$ fieldsresult and the constraint against double occupancy can be resolved. Thestaggered CP$^1$ fields are split into slow and fast modes, such that after agradient expansion, and after integrating out the fast modes and the dopantfermions, a CP$^1$ field-theory with a massive gauge field is obtained thatdescribes generically incommensurate coplanar magnetic structures, as discussedpreviously in the context of frustrated quantum antiferromagnets. Hence, thepossibility of deconfined spinons is opened by doping a colinearantiferromagnet.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Using a large sample of spiral galaxies for which 21 cm single-dish and/orlong-slit optical spectra are available, we make a detailed comparison betweenvarious estimates of rotational widths. Different optical width estimators areconsidered and their limitations discussed, with emphasis on biases associatedwith rotation curve properties (shape and extent) and disk central surfacebrightness. The best match with HI rotational velocities is obtained withPolyex widths, which are measured at the optical radius (encompassing a fixedfraction of the total light of the galaxy) from a model fit to the rotationcurve. In contrast with Polyex widths, optical rotational velocities measuredat 2.15 disk scale lengths r_d deviate from HI widths by an amount thatcorrelates with the central surface brightness of the disk. This bias occursbecause the rotation curves of galaxies are in general still rising at 2.15r_d, and the fraction of total mass contained within this radius decreases withincreasing disk surface brightness. Statistical corrections, parameterized bythe radial extent of the observed rotation curve, are provided to reduce Polyexand HI width measurements into a homogeneous system. This yields a singlerobust estimate of rotational velocity to be used for applications of diskscaling relations.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The notion of $\\times$-homotopy from \\cite{DocHom} is investigated in thecontext of the category of pointed graphs. The main result is a long exactsequence that relates the higher homotopy groups of the space $\\Hom_*(G,H)$with the homotopy groups of $\\Hom_*(G,H^I)$. Here $\\Hom_*(G,H)$ is a spacewhich parametrizes pointed graph maps from $G$ to $H$ (a pointed version of theusual $\\Hom$ complex), and $H^I$ is the graph of based paths in $H$. As acorollary it is shown that $\\pi_i \\big(\\Hom_*(G,H) \\big) \\cong [G,\\Omega^iH]_{\\times}$, where $\\Omega H$ is the graph of based closed paths in $H$ and$[G,K]_{\\times}$ is the set of $\\times$-homotopy classes of pointed graph mapsfrom $G$ to $K$. This is similar in spirit to the results of \\cite{BBLL}, wherethe authors seek a space whose homotopy groups encode a similarly definedhomotopy theory for graphs. The categorical connections to those constructionsare discussed.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The contact model for the spread of disease may be viewed as a directedpercolation model on $\\ZZ \\times \\RR$ in which the continuum axis is orientedin the direction of increasing time. Techniques from percolation have enabled afairly complete analysis of the contact model at and near its critical point.The corresponding process when the time-axis is unoriented is an undirectedpercolation model to which now standard techniques may be applied. One mayconstruct in similar vein a random-cluster model on $\\ZZ \\times \\RR$, withassociated continuum Ising and Potts models. These models are of independentinterest, in addition to providing a path-integral representation of thequantum Ising model with transverse field. This representation may be used toobtain a bound on the entanglement of a finite set of spins in the quantumIsing model on $\\ZZ$, where this entanglement is measured via the entropy ofthe reduced density matrix. The mean-field version of the quantum Ising modelgives rise to a random-cluster model on $K_n \\times \\RR$, thereby extending theErdos-Renyi random graph on the complete graph $K_n$.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "This paper investigates the use of evolutionary optimisation techniques toregister a template with a scene image. An error function is created to measurethe correspondence of the template to the image. The problem presented here isto optimise the horizontal, vertical and scaling parameters that register thetemplate with the scene. The Genetic Algorithm, Simulated Annealing andParticle Swarm Optimisations are compared to a Nelder-Mead Simplex optimisationwith starting points chosen in a pre-processing stage. The paper investigatesthe precision and accuracy of each method and shows that all four methodsperform favourably for image registration. SA is the most precise, GA is themost accurate. PSO is a good mix of both and the Simplex method returns localminima the most. A pre-processing stage should be investigated for theevolutionary methods in order to improve performance. Discrete versions of theoptimisation methods should be investigated to further improve computationalperformance.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We consider the Kalman - Yakubovich - Popov (KYP) inequality \\[\\begin{pmatrix} X-A^* XA-C^*C & -A^*X B- C^*D\\cr -B^*X A-D^* C & I- B^*X B-D^*D\\end{pmatrix} \\ge 0 \\] for contractive operator matrices $ \\begin{pmatrix}A&B\\cr C &D \\end{pmatrix}:\\begin{pmatrix}\\mathfrak{H}\\cr\\mathfrak{M}\\end{pmatrix}\\to\\begin{pmatrix}\\mathfrak{H}\\cr\\mathfrak{N} \\end{pmatrix}, $where $\\mathfrak{H},$ $\\mathfrak{M}$, and $\\mathfrak{N}$ are separable Hilbertspaces. We restrict ourselves to the solutions $X$ from the operator interval$[0, I_\\mathfrak{H}]$. Several equivalent forms of KYP are obtained. Using theparametrization of the blocks of contractive operator matrices, the Kre\\u{\\i}nshorted operator, and the M\\\"obius representation of the Schur classoperator-valued function we find several equivalent forms of the KYPinequality. Properties of solutions are established and it is proved that theminimal solution of the KYP inequality satisfies the corresponding algebraicRiccati equation and can be obtained by the iterative procedure with thespecial choice of the initial point. In terms of the Kre\\u{\\i}n shortedoperators a necessary condition and some sufficient conditions for uniquenessof the solution are established.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We provide a model for how Kennicutt-Schmidt (KS) laws, which describe thecorrelation between star formation rate and gas surface or volume density,depend on the molecular line chosen to trace the gas. We show that, for linesthat can be excited at low temperatures, the KS law depends on how the linecritical density compares to the median density in a galaxy's star-formingmolecular clouds. High critical density lines trace regions with similarphysical properties across galaxy types, and this produces a linear correlationbetween line luminosity and star formation rate. Low critical density linesprobe regions whose properties vary across galaxies, leading to a starformation rate that varies superlinearly with line luminosity. We show that asimple model in which molecular clouds are treated as isothermal and homogenouscan quantitatively reproduce the observed correlations between galacticluminosities in far infrared and in the CO(1->0) and HCN(1->0) lines, andnaturally explains why these correlations have different slopes. We predictthat IR-line luminosity correlations should change slope for galaxies in whichthe median density is close to the line critical density. This prediction maybe tested by observations of lines such as HCO^+(1->0) with intermediatecritical densities, or by HCN(1->0) observations of intensely star-forming highredshift galaxies with very high densities. Recent observations by Gao et al.hint at just such a change in slope. We argue that deviations from linearity inthe HCN(1->0)-IR correlation at high luminosity are consistent with theassumption of a constant star formation efficiency.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Temperature dependent impedance spectroscopy enables the many contributionsto the dielectric and resistive properties of condensed matter to bedeconvoluted and characterized separately. We have achieved this formultiferroic epitaxial thin films of BiFeO3 (BFO) and BiMnO3 (BMO), keyexamples of materials with strong magneto-electric coupling. We demonstratethat the true film capacitance of the epitaxial layers is similar to that ofthe electrode interface, making analysis of capacitance as a function of filmthickness necessary to achieve deconvolution. We modeled non-Debye impedanceresponse using Gaussian distributions of relaxation times and reveal thatconventional resistivity measurements on multiferroic layers may be dominatedby interface effects. Thermally activated charge transport models yieldedactivation energies of 0.60 eV +- 0.05 eV (BFO) and 0.25 eV +- 0.03 eV (BMO),which is consistent with conduction dominated by oxygen vacancies (BFO) andelectron hopping (BMO). The intrinsic film dielectric constants were determinedto be 320 +- 75 (BFO) and 450 +- 100 (BMO).", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We study the long term evolution of magnetic fields generated by acollisionless relativistic $e^+e^-$ shock which is initially unmagnetized. Our2D particle-in-cell numerical simulations show that downstream of such aWeibel-mediated shock, particle distributions are close to isotropic,relativistic Maxwellians, and the magnetic turbulence is highly intermittentspatially, with the non-propagating magnetic fields forming relatively isolatedregions with transverse dimension $\\sim 10-20$ skin depths. These structuresdecay in amplitude, with little sign of downstream merging. The fields startwith magnetic energy density $\\sim (0.1-0.2)$ of the upstream kinetic energywithin the shock transition, but rapid downstream decay drives the fields tomuch smaller values, below $10^{-3}$ of equipartition after $10^3$ skin depths.  In an attempt to construct a theory that follows field decay to these smallervalues, we explore the hypothesis that the observed damping is a variant ofLandau damping in an unmagnetized plasma. The model is based on the small valueof the downstream magnetic energy density, which suggests that particle orbitsare only weakly perturbed from straight line motion, if the turbulence ishomogeneous. Using linear kinetic theory applied to electromagnetic fields inan isotropic, relativistic Maxwellian plasma, we find a simple analytic formfor the damping rates, $\\gamma_k$, in two and three dimensions for smallamplitude, subluminous electromagnetic fields. We find that magnetic energydoes damp due to phase mixing of current carrying particles as $(\\omega_pt)^{-q}$ with $q \\sim 1$. (abridged)", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We investigate cooperative wireless relay networks in which the nodes canhelp each other in data transmission. We study different coding strategies inthe single-source single-destination network with many relay nodes. Given themyriad of ways in which nodes can cooperate, there is a natural routingproblem, i.e., determining an ordered set of nodes to relay the data from thesource to the destination. We find that for a given route, thedecode-and-forward strategy, which is an information theoretic cooperativecoding strategy, achieves rates significantly higher than that achievable bythe usual multi-hop coding strategy, which is a point-to-point non-cooperativecoding strategy. We construct an algorithm to find an optimal route (in termsof rate maximizing) for the decode-and-forward strategy. Since the algorithmruns in factorial time in the worst case, we propose a heuristic algorithm thatruns in polynomial time. The heuristic algorithm outputs an optimal route whenthe nodes transmit independent codewords. We implement these coding strategiesusing practical low density parity check codes to compare the performance ofthe strategies on different routes.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Capacity improvement from transmitter and receiver cooperation isinvestigated in a two-transmitter, two-receiver network with phase fading andfull channel state information available at all terminals. The transmitterscooperate by first exchanging messages over an orthogonal transmittercooperation channel, then encoding jointly with dirty paper coding. Thereceivers cooperate by using Wyner-Ziv compress-and-forward over an analogousorthogonal receiver cooperation channel. To account for the cost ofcooperation, the allocation of network power and bandwidth among the data andcooperation channels is studied. It is shown that transmitter cooperationoutperforms receiver cooperation and improves capacity over non-cooperativetransmission under most operating conditions when the cooperation channel isstrong. However, a weak cooperation channel limits the transmitter cooperationrate; in this case receiver cooperation is more advantageous.Transmitter-and-receiver cooperation offers sizable additional capacity gainover transmitter-only cooperation at low SNR, whereas at high SNR transmittercooperation alone captures most of the cooperative capacity improvement.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "In this paper, we report on the magnetic properties of Ba2CoS3, a spin-chaincompound recently found to be the first Co2+ containing one-dimensionalsulphide to show metallic-like conductivity and negative magnetoresistance. Wecarried out an in-depth experimental investigation of the local structure ofthe cobalt atoms, and ab-initio calculations of the resulting electronicconfiguration of Co2+. From theoretical considerations, the intra-chaincoupling was predicted to be antiferromagnetic. Experimentally, severalestimates of this magnetic coupling were derived by analysing the temperaturedependence of the magnetic susceptibility. Magnetic and heat capacitymeasurements also provided evidence of a three-dimensional antiferromagneticordering, a feature indicative of a noticeable inter-chain coupling in thisquasi-1D system.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Although the giant radiogalaxy M 87 harbors many distinct regions ofbroad-band nonthermal emission, the recently reported fast variability of TeVgamma rays from M 87 on a timescale of days strongly constrains the range ofspeculations concerning the possible sites and scenarios of particleacceleration responsible for the observed TeV emission. A natural productionsite of this radiation is the immediate vicinity of the central supermassivemass black hole (BH). Because of the low bolometric luminosity, the nucleus ofM 87 is effectively transparent for gamma rays up to energy of 10 TeV, whichmakes this source an ideal laboratory for study of particle accelerationprocesses close to the BH event horizon. We critically analyse differentpossible radiation mechanisms in this region, and argue that the observed veryhigh-energy gamma ray emission can be explained by the inverse Compton emissionof ultrarelativistic electron-positron pairs produced through the developmentof an electromagnetic cascade in the BH magnetosphere. We demonstrate, throughdetailed numerical calculations of acceleration and radiation of electrons inthe magnetospheric vacuum gap, that this ``pulsar magnetosphere like'' scenariocan satisfactorily explain the main properties of TeV gamma-ray emission of M87.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Protein-DNA complexes with loops play a fundamental role in a wide variety ofcellular processes, ranging from the regulation of DNA transcription totelomere maintenance. As ubiquitous as they are, their precise in vivoproperties and their integration into the cellular function still remainlargely unexplored. Here, we present a multilevel approach that efficientlyconnects in both directions molecular properties with cell physiology and useit to characterize the molecular properties of the looped DNA-lac repressorcomplex while functioning in vivo. The properties we uncover include thepresence of two representative conformations of the complex, the stabilizationof one conformation by DNA architectural proteins, and precise values of theunderlying twisting elastic constants and bending free energies. Incorporationof all this molecular information into gene-regulation models reveals anunprecedented versatility of looped DNA-protein complexes at shaping theproperties of gene expression.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The stability of two-dimensional (2D) layers and membranes is subject of along standing theoretical debate. According to the so called Mermin-Wagnertheorem, long wavelength fluctuations destroy the long-range order for 2Dcrystals. Similarly, 2D membranes embedded in a 3D space have a tendency to becrumpled. These dangerous fluctuations can, however, be suppressed byanharmonic coupling between bending and stretching modes making that atwo-dimensional membrane can exist but should present strong heightfluctuations. The discovery of graphene, the first truly 2D crystal and therecent experimental observation of ripples in freely hanging graphene makesthese issues especially important. Beside the academic interest, understandingthe mechanisms of stability of graphene is crucial for understanding electronictransport in this material that is attracting so much interest for its unusualDirac spectrum and electronic properties. Here we address the nature of theseheight fluctuations by means of straightforward atomistic Monte Carlosimulations based on a very accurate many-body interatomic potential forcarbon. We find that ripples spontaneously appear due to thermal fluctuationswith a size distribution peaked around 70 \\AA which is compatible withexperimental findings (50-100 \\AA) but not with the current understanding ofstability of flexible membranes. This unexpected result seems to be due to themultiplicity of chemical bonding in carbon.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Theory of magnetic deflagration (avalanches) in crystals of molecular magnetshas been developed. The phenomenon resembles the burning of a chemicalsubstance, with the Zeeman energy playing the role of the chemical energy.Non-destructive reversible character of magnetic deflagration, as well as thepossibility to continuously tune the flammability of the crystal by changingthe magnetic field, makes molecular magnets an attractive toy system for adetailed study of the burning process. Besides simplicity, new features, ascompared to the chemical burning, include possibility of quantum decay ofmetastable spin states and strong temperature dependence of the heat capacityand thermal conductivity. We obtain analytical and numerical solutions forcriteria of the ignition of magnetic deflagration, and compute the ignitionrate and the speed of the developed deflagration front.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "AIM: We have recently developed a microscopic Monte Carlo approach to studysurface chemistry on interstellar grains and the morphology of ice mantles. Themethod is designed to eliminate the problems inherent in the rate-equationformalism to surface chemistry. Here we report the first use of this method ina chemical model of cold interstellar cloud cores that includes both gas-phaseand surface chemistry. The surface chemical network consists of a small numberof diffusive reactions that can produce molecular oxygen, water, carbondioxide, formaldehyde, methanol and assorted radicals. METHOD: The simulationis started by running a gas-phase model including accretion onto grains but nosurface chemistry or evaporation. The starting surface consists of either flator rough olivine. We introduce the surface chemistry of the three species H, Oand CO in an iterative manner using our stochastic technique. Under theconditions of the simulation, only atomic hydrogen can evaporate to asignificant extent. Although it has little effect on other gas-phase species,the evaporation of atomic hydrogen changes its gas-phase abundance, which inturn changes the flux of atomic hydrogen onto grains. The effect on the surfacechemistry is treated until convergence occurs. We neglect all non-thermaldesorptive processes. RESULTS: We determine the mantle abundances of assortedmolecules as a function of time through 2x10^5 yr. Our method also allowsdetermination of the abundance of each molecule in specific monolayers. Themantle results can be compared with observations of water, carbon dioxide,carbon monoxide, and methanol ices in the sources W33A and Elias 16. Other thana slight underproduction of mantle CO, our results are in very good agreementwith observations.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present the results of our investigation of the intermediate-age starcluster BS 90, located in the vicinity of the HII region N 66 in the SMC,observed with HST/ACS. The high-resolution data provide a unique opportunityfor a very detailed photometric study performed on one of the rareintermediate-age rich SMC clusters. The complete set of observations iscentered on the association NGC 346 and contains almost 100,000 stars down to V~28 mag. In this study we focus on the northern part of the region, whichcovers almost the whole stellar content of BS 90. We construct its stellarsurface density profile and derive structural parameters. Isochrone fits on theCMD of the cluster results in an age of about 4.5 Gyr. The luminosity functionis constructed and the present-day mass function of BS 90 has been obtainedusing the mass-luminosity relation, derived from the isochrone models. We founda slope between -1.30 and -0.95, comparable or somewhat shallower than atypical Salpeter IMF. Examination of the radial dependence of the mass functionshows a steeper slope at larger radial distances, indicating mass segregationin the cluster. The derived half-mass relaxation time of 0.95 Gyr suggests thatthe cluster is mass segregated due to its dynamical evolution. From theisochrone model fits we derive a metallicity for BS 90 of [Fe/H]=-0.72, whichadds an important point to the age-metallicity relation of the SMC. We discussour findings on this relation in comparison to other SMC clusters.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Heavy-quark jets are important in many of today's collider studies andsearches, yet predictions for them are subject to much larger uncertaintiesthan for light jets. This is because of strong enhancements in higher ordersfrom large logarithms, ln(p_t/m_Q). We propose a new definition of heavy-quarkjets, which is free of final-state logarithms to all orders and such that allinitial-state collinear logarithms can be resummed into the heavy-quark partondistributions. Heavy-jet spectra can then be calculated in the masslessapproximation, which is simpler than a massive calculation and reduces thetheoretical uncertainties by a factor of three. This provides the first everaccurate predictions for inclusive b- and c-jets, and the latter havesignificant discriminatory power for the intrinsic charm content of the proton.The techniques introduced here could be used to obtain heavy-flavour jetresults from existing massless next-to-leading order calculations for a widerange of processes. We also discuss the experimental applicability of ourflavoured jet definition.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "High resolution optical and ultraviolet spectra of two B-type post-AsymptoticGiant Branch (post-AGB) stars in globular clusters, Barnard 29 in M 13 and ROA5701 in omega Cen, have been analysed using model atmosphere techniques. Theoptical spectra have been obtained with FEROS on the ESO 2.2-m telescope andthe 2d-Coud\\'e spectrograph on the 2.7-m McDonald telescope, while theultraviolet observations are from the GHRS on the HST. Abundances of lightelements (C, N, O, Mg, Al and S) plus Fe have been determined from the opticalspectra, while the ultraviolet data provide additional Fe abundance estimatesfrom Fe III absorption lines in the 1875-1900 {\\AA} wavelength region. Ageneral metal underabundance relative to young B-type stars is found for bothBarnard 29 and ROA 5701. These results are consistent with the metallicities ofthe respective clusters, as well as with previous studies of the objects. Thederived abundance patterns suggest that the stars have not undergone a gas-dustseparation, contrary to previous suggestions, although they may have evolvedfrom the AGB before the onset of the third dredge-up. However, the Feabundances derived from the HST spectra are lower than those expected from themetallicities of the respective clusters, by 0.5 dex for Barnard 29 and 0.8 dexfor ROA 5701. A similar systematic underabundance is also found for otherB-type stars in environments of known metallicity, such as the MagellanicClouds. These results indicate that the Fe III ultraviolet lines may yieldabundance values which are systematically too low by typically 0.6 dex andhence such estimates should be treated with caution.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We construct a new random probability measure on the sphere and on the unitinterval which in both cases has a Gibbs structure with the relative entropyfunctional as Hamiltonian. It satisfies a quasi-invariance formula with respectto the action of smooth diffeomorphism of the sphere and the intervalrespectively. The associated integration by parts formula is used to constructtwo classes of diffusion processes on probability measures (on the sphere orthe unit interval) by Dirichlet form methods. The first one is closely relatedto Malliavin's Brownian motion on the homeomorphism group. The second one is aprobability valued stochastic perturbation of the heat flow, whose intrinsicmetric is the quadratic Wasserstein distance. It may be regarded as thecanonical diffusion process on the Wasserstein space.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Any stretching of Ringel's non-Pappus pseudoline arrangement when projectedinto the Euclidean plane, implicitly contains a particular arrangement of ninetriangles. This arrangement has a complex constraint involving the sines of itsangles. These constraints cannot be satisfied by any projection of the initialarrangement. This is sufficient to prove Pappus's theorem. The derivation ofthe constraint is via systems of inequalities arising from the polarcoordinates of the lines. These systems are linear in r for any given theta,and their solubility can be analysed in terms of the signs of determinants. Theevaluation of the determinants is via a normal form for sums of products ofsines, giving a powerful system of trigonometric identities. The particularresult is generalized to arrangements derived from three edge connected totallycyclic directed graphs, conjectured to be sufficient for a complete analysis ofangle constraining arrangements of lines, and thus a full response to Ringel'sslope conjecture. These methods are generally applicable to the realizabilityproblem for rank 3 oriented matroids.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We report a detection of the 9.7 micrometer silicate absorption feature in adamped Lyman-alpha (DLA) system at z_{abs} = 0.524 toward AO0235+164, using theInfrared Spectrograph (IRS) onboard the Spitzer Space Telescope. The featureshows a broad shallow profile over about 8-12 micrometers in the absorber restframe and appears to be > 15 sigma significant in equivalent width. The featureis fit reasonably well by the silicate absorption profiles for laboratoryamorphous olivine or diffuse Galactic interstellar clouds. To our knowledge,this is the first indication of 9.7 micrometer silicate absorption in a DLA. Wediscuss potential implications of this finding for the nature of the dust inquasar absorbers. Although the feature is relatively shallow (tau_{9.7} =0.08-0.09), it is about 2 times deeper than expected from extrapolation of thetau_{9.7} vs. E(B-V) relation known for diffuse Galactic interstellar clouds.Further studies of the 9.7 micrometer silicate feature in quasar absorbers willopen a new window on the dust in distant galaxies.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Tseytlin has recently proposed that an action functional exists whosegradient generates to all orders in perturbation theory the RenormalizationGroup (RG) flow of the target space metric in the worldsheet sigma model. Thegradient is defined with respect to a metric on the space of coupling constantswhich is explicitly known only to leading order in perturbation theory, but atthat order is positive semi-definite, as follows from Perelman's work on theRicci flow. This gives rise to a monotonicity formula for the flow which isexpected to fail only if the beta function perturbation series fails toconverge, which can happen if curvatures or their derivatives grow large. Wetest the validity of the monotonicity formula at next-to-leading order inperturbation theory by explicitly computing the second-order terms in themetric on the space of coupling constants. At this order, this metric is foundnot to be positive semi-definite. In situations where this might spoilmonotonicity, derivatives of curvature become large enough for higher orderperturbative corrections to be significant.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "SQUID magnetometry and polarised neutron reflectivity measurements have beenemployed to characterise the magnetic properties of U/Fe, U/Co and U/Gdmultilayers. The field dependence of the magnetisation was measured at 10K inmagnetic fields from -70kOe to 70kOe. A temperature dependent study of themagnetisation evolution was undertaken for a selection of U/Gd samples. PNR wascarried out in a field of 4.4kOe for U/Fe and U/Co samples (at roomtemperature) and for U/Gd samples (at 10K). Magnetic 'dead' layers of about 15Angstrom were observed for U/Fe and U/Co samples, consistent with a picture ofinterdiffused interfaces. A large reduction in the magnetic moment, constantover a wide range of Gd layer thicknesses, was found for the U/Gd system (about4 Bohr magnetons compared with 7.63 for the bulk metal). This could beunderstood on the basis of a pinning of Gd moments arising from a column-likegrowth mechanism of the Gd layers. A study of the effective anisotropy suggeststhat perpendicular magnetic anisotropy could occur in multilayers consisting ofthick U and thin Gd layers. A reduction in the Curie temperature was observedas a function of Gd layer thickness, consistent with a finite-size scalingbehaviour.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "In this paper we study a novel spin chain with nearest-neighbors interactionsdepending on the sites coordinates, which in some sense is intermediate betweenthe Heisenberg chain and the spin chains of Haldane-Shastry type. We show thatwhen the number of spins is sufficiently large both the density of sites andthe strength of the interaction between consecutive spins follow the Gaussianlaw. We develop an extension of the standard freezing trick argument thatenables us to exactly compute a certain number of eigenvalues and theircorresponding eigenfunctions. The eigenvalues thus computed are all integers,and in fact our numerical studies evidence that these are the only integereigenvalues of the chain under consideration. This fact suggests that thischain can be regarded as a finite-dimensional analog of the class ofquasi-exactly solvable Schroedinger operators, which has been extensivelystudied in the last two decades. We have applied the method of moments to studysome statistical properties of the chain's spectrum, showing in particular thatthe density of eigenvalues follows a Wigner-like law. Finally, we emphasizethat, unlike the original freezing trick, the extension thereof developed inthis paper can be applied to spin chains whose associated dynamical spin modelis only quasi-exactly solvable.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The Stanley lattice, Tamari lattice and Kreweras lattice are three remarkableorders defined on the set of Catalan objects of a given size. These latticesare ordered by inclusion: the Stanley lattice is an extension of the Tamarilattice which is an extension of the Kreweras lattice. The Stanley order can bedefined on the set of Dyck paths of size $n$ as the relation of \\emph{beingabove}. Hence, intervals in the Stanley lattice are pairs of non-crossing Dyckpaths. In a former article, the second author defined a bijection $\\Phi$between pairs of non-crossing Dyck paths and the realizers of triangulations(or Schnyder woods). We give a simpler description of the bijection $\\Phi$.Then, we study the restriction of $\\Phi$ to Tamari's and Kreweras' intervals.We prove that $\\Phi$ induces a bijection between Tamari intervals and minimalrealizers. This gives a bijection between Tamari intervals and triangulations.We also prove that $\\Phi$ induces a bijection between Kreweras intervals andthe (unique) realizers of stack triangulations. Thus, $\\Phi$ induces abijection between Kreweras intervals and stack triangulations which are knownto be in bijection with ternary trees.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "To understand the whole set of positive and null data on theTheta+(1530)-production, we suggest the hypothesis that multiquark hadrons aremainly generated from many-quark states, which emerge either as short-termhadron fluctuations, or as hadron remnants in hard processes. This approachallows us to describe both non-observation of the Theta+ in current nullexperiments and peculiar features of its production in positive experiments.Further, we are able to propose new experiments that might be decisive for theproblem of the Theta+ existence. Distributions of the Theta+ in suchexperiments can give important information both on higher Fock components ofconventional hadrons and about structure and hadronization properties of hadronremnants produced in hard processes. We also explain that description ofmultiquark hadrons may require a modified form of the constituent quark model,with quark masses and couplings being intermediate between their values for thefamiliar constituent quarks and the current ones.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We calculate the CP averaged branching ratios and CP-violating asymmetriesfor $B_s^0 \\to \\eta \\eta, \\eta \\eta^\\prime$ and $\\eta^\\prime \\eta^\\prime$decays in the perturbative QCD (pQCD) approach here. The pQCD predictions forthe CP-averaged branching ratios are $Br(B_s^0 \\to \\eta \\eta) = \\left(14.2^{+18.0}_{-7.5}) \\times 10^{-6}$, $Br(B_s^0 \\to \\eta \\eta^\\prime)= \\left(12.4 ^{+18.2}_{-7.0}) \\times 10^{-6}$, and $Br(B_s^0 \\to \\eta^{\\prime}\\eta^{\\prime}) = \\left (9.2^{+15.3}_{-4.9}) \\times 10^{-6}$, which agree wellwith those obtained by employing the QCD factorization approach and also beconsistent with available experimental upper limits. The gluonic contributionsare small in size: less than 7% for $B_s \\to \\eta \\eta$ and $ \\eta \\eta^\\prime$decays, and around 18% for $B_s \\to \\eta' \\eta'$ decay. The CP-violatingasymmetries for three decays are very small: less than 3% in magnitude.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We investigate dynamical systems characterized by a time series of distinctsemi-stable activity patterns, as they are observed in cortical neural activitypatterns. We propose and discuss a general mechanism allowing for an adiabaticcontinuation between attractor networks and a specific adjoined transient-statenetwork, which is strictly dissipative. Dynamical systems with transient statesretain functionality when their working point is autoregulated; avoidingprolonged periods of stasis or drifting into a regime of rapid fluctuations. Weshow, within a continuous-time neural network model, that a single localupdating rule for online learning allows simultaneously (i) for informationstorage via unsupervised Hebbian-type learning, (ii) for adaptive regulation ofthe working point and (iii) for the suppression of runaway synaptic growth.Simulation results are presented; the spontaneous breaking of time-reversalsymmetry and link symmetry are discussed.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We describe azimuth structure commonly associated with elliptic and directedflow in the context of 2D angular autocorrelations for the purpose of preciseseparation of so-called nonflow (mainly minijets) from flow. We extend theFourier-transform description of azimuth structure to include power spectra andautocorrelations related by the Wiener-Khintchine theorem. We analyze severalexamples of conventional flow analysis in that context and question therelevance of reaction plane estimation to flow analysis. We introduce the 2Dangular autocorrelation with examples from data analysis and describe asimulation exercise which demonstrates precise separation of flow and nonflowusing the 2D autocorrelation method. We show that an alternative correlationmeasure based on Pearson's normalized covariance provides a more intuitivemeasure of azimuth structure.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Recently [J. Haro and E. Elizalde, Phys. Rev. Lett. {\\bf 97}, 130401 (2006)],a Hamiltonian formulation has been introduced in order to address somelongstanding severe problems associated with the physical description of thedynamical Casimir effect at all times while the mirrors are moving. Here wepresent the complete calculation providing precise details, in particular, ofthe regularization procedure, which is decisive for the correct derivation ofphysically meaningful quantities. A basic difference when comparing with theresults previously obtained by other authors is the fact that the motion forcederived in our approach contains a reactive term --proportional to the mirrors'acceleration. This is of the essence in order to obtain particles with apositive energy all the time during the oscillation of the mirrors --whilealways satisfying the energy conservation law. A careful analysis of theinterrelations among the different results previously obtained in theliterature is then carried out. For simplicity, the specific case of a neutralscalar field in one dimension, with one or two partially transmitting mirrors(a fundamental proviso for the regularization issue) is considered in moredetail, but our general method is shown to be generalizable, without essentialproblems (Sect. 2 of this paper), to fields of any kind in two and higherdimensions.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "In the present work we compare in detail some of the major theoreticallibraries with observations, aiming at detecting weaknesses and strengths fromthe stellar population modelling point of view. We compared model predictionsand observations for broad- band colours and for high resolution spectralfeatures. Concerning the broad-band colours, we measured the stellar colourgiven by three recent sets of model atmospheres and flux distributions(Castelli& Kurucz 2003; Gustafsson et al. 2003; Brott & Hauschildt 2005), and comparedthem with a recent UBVRIJHK calibration (Worthey & Lee 2007). We found that themodels can reproduce with reasonable accuracy the stellar colours for a fairinterval in effective temperatures and gravities. The exceptions are: 1) theU-B colour, where the models are typically redder than the observations, and;2) the very cool stars in general (V-K > ~3).Concerning the high resolutionfeatures, we measured 35 spectral indices defined in the literature on threehigh resolution synthetic libraries (Coelho et al. 2005; Martins et al. 2005;Munari et al. 2005), and compared them with the observed measurements given bythree empirical libraries (Valdes et al.2004; Sanchez-Blazquez et al. 2006;Prugniel & Soubiran 2001). We found that the direct comparison between modelsand observations is not a simple task, given the uncertainties in parameterdeterminations of empirical libraries. Taking that aside, we found that ingeneral the three libraries present similar behaviours and systematicdeviations. For stars with Teff < 7000K, the library by Coelho et al. (2005) isthe one with best average performance. We detect that lists of atomic andmolecular line opacities still need improvement, specially in the blue regionof thespectrum, and for the cool stars (Teff < ~4500K).", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We analyze the scaling parameter, extracted from the fidelity for twodifferent ground states, for the one-dimensional quantum Ising model in atransverse field near the critical point. It is found that, in thethermodynamic limit, the scaling parameter is singular, and the derivative ofits logarithmic function with respect to the transverse field strength islogarithmically divergent at the critical point. The scaling behavior isconfirmed numerically by performing a finite size scaling analysis for systemsof different sizes, consistent with the conformal invariance at the criticalpoint. This allows us to extract the correlation length critical exponent,which turns out to be universal in the sense that the correlation lengthcritical exponent does not depend on either the anisotropic parameter or thetransverse field strength.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Yield design formulation for porous media subjected to flow, usingapproximate pressure field. We attempt here to use the kinematic method ofyield design in the case of a porous medium subjected to flow (with or withoutfree surface), without looking for the exact solution of the pressure field.The method proposed here is based on the use of approximate pressure fields. Inthis paper, we show how, under different conditions concerning the yieldcriterion and the velocity field, the use of such approximate fields allows toobtain a necessary condition for stability without having to find the realpressure field. Nous cherchons ici \\`a utiliser la m\\'ethode cin\\'ematique ducalcul \\`a la rupture dans le cas d'un milieu poreux soumis \\`a un \\'ecoulementavec ou sans surface libre sans conna\\^itre la solution exacte du champ depression. La m\\'ethode propos\\'ee ici repose sur l'utilisation de champs depression approch\\'es par d\\'efaut. Nous montrerons comment sous certainesconditions portant sur le crit\\`ere de r\\'esistance et sur le champ de vitesseutilis\\'e, l'utilisation de tels champs de pression approch\\'es permetd'obtenir une condition n\\'ecessaire de stabilit\\'e sans avoir \\`a d\\'eterminerexactement l'\\'ecoulement.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Dissipation-free current transport in high-temperature superconductors is oneof the most crucial properties of this class of materials which is directlyrelated to the effective inhibition of flux line movement by defect structures.In this respect epitaxially grown thin films of YBa2Cu3O7-d (YBCO) are provingto be the strongest candidates for many widescale applications that are closeto realization. We show that the relation between different defect structuresand flux line pinning in these films exhibits universal features which areclearly displayed in a detailed analysis of the temperature-dependent behaviourof local critical currents. This allows us to identify different pinningmechanisms at different temperatures to be responsible for the found criticalcurrents. Additionally, the presence of grain boundaries with very lowmisorientation angles affects the temperature stability of the criticalcurrents which has important consequences for future applications.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "INTEGRAL monitoring of the Galactic Plane is revealing a growing number ofrecurrent X-ray transients, characterised by short outbursts with very fastrise times (~ tens of minutes) and typical durations of a few hours. Asubstantial fraction of these sources are associated with OB supergiants andhence define a new class of massive X-ray binaries, which we call SupergiantFast X-ray Transients. Characterisation of the astrophysical parameters oftheir counterparts is underway. So far, we have found a number of late O andearly B supergiants of different luminosities at a large range of distances.Nothing in their optical properties sets them apart from classical SupergiantX-ray Binaries. On the other hand, there is now rather concluding evidence thatpersistent supergiant X-ray binaries also show fast outbursts. This suggests acontinuum of behaviours between typical persistent supergiant systems andpurely transient systems, but offers very little information about the physicalcauses of the outbursts.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We continue our study of chaotic mixing and transport of passive particles ina simple model of a meandering jet flow [Prants, et al, Chaos {\\bf 16}, 033117(2006)]. In the present paper we study and explain phenomenologically aconnection between dynamical, topological, and statistical properties ofchaotic mixing and transport in the model flow in terms of dynamical traps,singular zones in the phase space where particles may spend arbitrary long butfinite time [Zaslavsky, Phys. D {\\bf 168--169}, 292 (2002)]. The transport ofpassive particles is described in terms of lengths and durations of zonalflights which are events between two successive changes of sign of zonalvelocity. Some peculiarities of the respective probability density functionsfor short flights are proven to be caused by the so-called rotational-islandstraps connected with the boundaries of resonant islands (including those of thevortex cores) filled with the particles moving in the same frame. Whereas, thestatistics of long flights can be explained by the influence of the so-calledballistic-islands traps filled with the particles moving from a frame to frame.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We report on the transport and magnetic properties of hybrid trilayers andbilayers that consist of low spin-polarized Ni80Fe20 exhibiting in-plane but nouniaxial anisotropy and low-Tc Nb. We reveal a magnetoresistance effect that ispronounced. In our trilayers the magnetoresistance exhibits an increase of twoorders of magnitude when the superconducting state is reached: from theconventional normal-state values 0.6 % it goes up to 1000 % for temperaturesbelow Tc. In contrast, in the bilayers the effect is only minor since from 3%in the normal state increases only to 70 % for temperatures below Tc.Magnetization data of both the longitudinal and transverse magnetic componentsare presented. Most importantly, we present data not only for the normal stateof Nb but also in its superconducting state. Strikingly, these data show thatbelow its Tc SC the Nb interlayer under the influence of the outer Ni80Fe20layers attains a magnetization component transverse to the external field. Bycomparing the transport and magnetization data we propose a candidate mechanismthat could motivate the pronounced magnetoresistance effect observed in thetrilayers. Adequate magnetostatic coupling of the outer Ni80Fe20 layers ismotivated by stray fields that emerge naturally in their whole surface due tothe multidomain magnetic structure that they attain near coercivity. Atomicforce microscopy is employed in order to examine the possibility that suchmagnetostatic coupling could be promoted by interface roughness. Referring tothe bilayers, although out-of-plane rotation of the magnetization of the singleNi80Fe20 layer is still observed, in these structures magnetostatic couplingdoes not occur due to the absence of a second Ni80Fe20 one so that the observedmagnetoresistance peaks are only modest.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The dynamical discrete web (DDW), introduced in recent work of Howitt andWarren, is a system of coalescing simple symmetric one-dimensional random walkswhich evolve in an extra continuous dynamical parameter s. The evolution is byindependent updating of the underlying Bernoulli variables indexed by discretespace-time that define the discrete web at any fixed s. In this paper, we studythe existence of exceptional (random) values of s where the paths of the web donot behave like usual random walks and the Hausdorff dimension of the set ofsuch exceptional s. Our results are motivated by those about exceptional timesfor dynamical percolation in high dimension by H\\\"aggstrom, Peres and Steif,and in dimension two by Schramm and Steif. The exceptional behavior of thewalks in DDW is rather different from the situation for dynamical random walksof Benjamini, H\\\"aggstrom, Peres and Steif. In particular, we prove that thereare exceptional values of s for which the walk from the origin S^s(n) haslimsup S^s(n)/\\sqrt n \\leq K with a nontrivial dependence of the Hausdorffdimension on K. We also discuss how these and other results extend to thedynamical Brownian web, a natural scaling limit of DDW. The scaling limit isthe focus of a paper in preparation; it was studied by Howitt and Warren and isrelated to the Brownian net of Sun and Swart.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "For positive semidefinite matrices $A$ and $B$, Ando and Zhan proved theinequalities $||| f(A)+f(B) ||| \\ge ||| f(A+B) |||$ and $||| g(A)+g(B) ||| \\le||| g(A+B) |||$, for any unitarily invariant norm, and for any non-negativeoperator monotone $f$ on $[0,\\infty)$ with inverse function $g$. Theseinequalities have very recently been generalised to non-negative concavefunctions $f$ and non-negative convex functions $g$, by Bourin and Uchiyama,and Kosem, respectively.  In this paper we consider the related question whether the inequalities $|||f(A)-f(B) ||| \\le ||| f(|A-B|) |||$, and $||| g(A)-g(B) ||| \\ge ||| g(|A-B|)|||$, obtained by Ando, for operator monotone $f$ with inverse $g$, also have asimilar generalisation to non-negative concave $f$ and convex $g$. We answerexactly this question, in the negative for general matrices, and affirmativelyin the special case when $A\\ge ||B||$.  In the course of this work, we introduce the novel notion of $Y$-dominatedmajorisation between the spectra of two Hermitian matrices, where $Y$ is itselfa Hermitian matrix, and prove a certain property of this relation that allowsto strengthen the results of Bourin-Uchiyama and Kosem, mentioned above.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The Hamiltonian approach to the General Relativity and the Standard Model isstudied in the context of its consistency with the Newton law, the Higgseffect, the Hubble cosmological evolution and the Cosmic Microwave Backgroundradiation physics.  The version of the Higgs potential is proposed, where its constant parameteris replaced by the dynamic zeroth Fourier harmonic of the very Higgs field. Inthis model, the extremum of the Coleman--Weinberg effective potential obtainedfrom the unit vacuum--vacuum transition amplitude immediately predicts mass ofHiggs field and removes tremendous vacuum cosmological density.  We show that the relativity principles unambiguously treat the Planck epoch,in the General Relativity, as the present-day one. It was shown that there areinitial data of the Electro-Weak epoch compatible with supposition that allparticles in the Universe are final products of decays of primordial Higgsparticles and W-, Z-vector bosons created from vacuum at the instant treated asthe \"Big-Bang\".", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We develop distributed algorithms to allocate resources in multi-hop wirelessnetworks with the aim of minimizing total cost. In order to observe thefundamental duplexing constraint that co-located transmitters and receiverscannot operate simultaneously on the same frequency band, we first devise aspectrum allocation scheme that divides the whole spectrum into multiplesub-bands and activates conflict-free links on each sub-band. We show that theminimum number of required sub-bands grows asymptotically at a logarithmic ratewith the chromatic number of network connectivity graph. A simple distributedand asynchronous algorithm is developed to feasibly activate links on theavailable sub-bands. Given a feasible spectrum allocation, we then designnode-based distributed algorithms for optimally controlling the transmissionpowers on active links for each sub-band, jointly with traffic routes and userinput rates in response to channel states and traffic demands. We show thatunder specified conditions, the algorithms asymptotically converge to theoptimal operating point.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We propose and study a model with glassy behavior. The state space of themodel is given by all triangulations of a sphere with $n$ nodes, half of whichare red and half are blue. Red nodes want to have 5 neighbors while blue oneswant 7. Energies of nodes with different numbers of neighbors are supposed tobe positive. The dynamics is that of flipping the diagonal of two adjacenttriangles, with a temperature dependent probability. We show that this systemhas an approach to a steady state which is exponentially slow, and show thatthe stationary state is unordered. We also study the local energy landscape andshow that it has the hierarchical structure known from spin glasses. Finally,we show that the evolution can be described as that of a rarefied gas withspontaneous generation of particles and annihilating collisions.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "``Top--down'' models explain the observation of ultra high energy cosmic rays(UHECR; $E \\gsim 5 \\cdot 10^{19}$ eV) through the decay of very massive,long--lived ``$X$ particles''. If superparticles with masses near a TeV exist,$X$ decays also lead to a significant flux of very energetic neutralinos,assumed to be the (stable or long--lived) lightest superparticles. There is arange of energies where neutrinos get absorbed in the Earth, but neutralinoscan still traverse it. These neutralinos could in principle be detected. Wecalculate the detection rate in planned experiments such as OWL and EUSO. Forbino--like neutralinos, which have been considered previously, we finddetection rates below 1 event per Teraton of target and year in all cases;often the rates are much smaller. In contrast, if the neutralino ishiggsino--like, more than ten events per year per Teraton might be observed, ifthe mass of the $X$ particle is near its lower bound of $\\sim 10^{12}$ GeV.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "While ferromagnetism at relatively high temperatures is seen in dilutedmagnetic semiconductors such as Ga_(1-x)Mn_(x)As, doped semiconductors withoutmagnetic ions have not shown evidence for ferromagnetism. Using a generalizeddisordered Hubbard model designed to characterize hydrogenic centers insemiconductors, we find that such systems may also exhibit a ferromagneticground state, at least on the nanoscale. This is found most clearly in a regimeinaccessible to bulk systems, but attainable in quantum dots as well asheterostructures. We present numerical results demonstrating the occurrence ofhigh spin ground states in both lattice and positionally disordered systems. Weexamine how the magnetic phases are affected by characteristics of real dopedsemiconductors, such as positional disorder and electron-hole asymmetry.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Halo samples that have no kinematic bias have been successfully isolated byphotometric observations. We show that the near-UV (NUV) magnitude of the GALEXAll-Sky Survey can be used, together with Johnson BV magnitudes in a (NUV-V)_0vs. (B-V)_0 plot, to distinguish blue horizontal branch (BHB) from other Astars of the same B-V color for 12<V<18. In addition, we use SDSS gr magnitudesin a (NUV - r)_0 vs. (g-r)_0 plot for 14<r<18. The faint limit will be extendedby ~3 magnitudes for the GALEX Medium-Deep Survey. Attempts to use NUV inconjunction with 2MASS magnitudes and ROTSE m_r magnitudes did not proveuseful. The (NUV - V)_0 vs. (B-V)_0 plot was used to examine BHB starcandidates of varying quality near the South Galactic Pole. We conclude thatthe addition of the GALEX NUV significantly adds to the reliabilty with whichthese stars can be identified.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present a theoretical framework for plasma turbulence in astrophysicalplasmas (solar wind, interstellar medium, galaxy clusters, accretion disks).The key assumptions are that the turbulence is anisotropic with respect to themean magnetic field and frequencies are low compared to the ion cyclotronfrequency. The energy injected at the outer scale scale has to be convertedinto heat, which ultimately cannot be done without collisions. A KINETICCASCADE develops that brings the energy to collisional scales both in space andvelocity. Its nature depends on the physics of plasma fluctuations. In each ofthe physically distinct scale ranges, the kinetic problem is systematicallyreduced to a more tractable set of equations. In the \"inertial range\" above theion gyroscale, the kinetic cascade splits into a cascade of Alfvenicfluctuations, which are governed by the RMHD equations at both the collisionaland collisionless scales, and a passive cascade of compressive fluctuations,which obey a linear kinetic equation along the moving field lines associatedwith the Alfvenic component. In the \"dissipation range\" between the ion andelectron gyroscales, there are again two cascades: the kinetic-Alfven-wave(KAW) cascade governed by two fluid-like Electron RMHD equations and a passivephase-space cascade of ion entropy fluctuations. The latter cascade brings theenergy of the inertial-range fluctuations that was damped by collisionlesswave-particle interaction at the ion gyroscale to collisional scales in thephase space and leads to ion heating. The KAW energy is similarly damped at theelectron gyroscale and converted into electron heat. Kolmogorov-style scalingrelations are derived for these cascades. Astrophysical and space-physicalapplications are discussed in detail.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The dynamics of many socioeconomic systems is determined by the decisionmaking process of agents. The decision process depends on agent'scharacteristics, such as preferences, risk aversion, behavioral biases, etc..In addition, in some systems the size of agents can be highly heterogeneousleading to very different impacts of agents on the system dynamics. The largesize of some agents poses challenging problems to agents who want to controltheir impact, either by forcing the system in a given direction or by hidingtheir intentionality. Here we consider the financial market as a model system,and we study empirically how agents strategically adjust the properties oflarge orders in order to meet their preference and minimize their impact. Wequantify this strategic behavior by detecting scaling relations of allometricnature between the variables characterizing the trading activity of differentinstitutions. We observe power law distributions in the investment timehorizon, in the number of transactions needed to execute a large order and inthe traded value exchanged by large institutions and we show that heterogeneityof agents is a key ingredient for the emergence of some aggregate propertiescharacterizing this complex system.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We propose a new concept for a very low background multi-ton liquid xenonDark Matter experiment. The detector consists of two concentric spheres and acharge readout device in the centre. Xenon between the two spheres forms aself-shield and veto device. The inner surface of the central sphere is coatedwith CsI to form an internal photocathode with minimum of 2\\pi coverage for anyevent in the active volume. Photoelectrons from the CsI photocathode drifttoward the charge readout micro-structure in the centre of the detector. Bothscintillation and ionisation are measured simultaneously for backgroundrejection and 3-D event mapping. In addition to external shielding, the lowbackground is achieved by eliminating PMTs and by using low radioactivity purematerials throughout the detector. We present detailed calculations of thecharge readout system and design details. The detector is expected to probe thefull SUSY parameter space.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Aims. This work presents a new hydrodynamical algorithm to studyastrophysical detonations. A prime motivation of this development is thedescription of a carbon detonation in conditions relevant to superbursts, whichare thought to result from the propagation of a detonation front around thesurface of a neutron star in the carbon layer underlying the atmosphere.Methods. The algorithm we have developed is a finite-volume method inspired bythe original MUSCL scheme of van Leer (1979). The algorithm is of second-orderin the smooth part of the flow and avoids dimensional splitting. It is appliedto some test cases, and the time-dependent results are compared to thecorresponding steady state solution. Results. Our algorithm proves to be robustto test cases, and is considered to be reliably applicable to astrophysicaldetonations. The preliminary one-dimensional calculations we have performeddemonstrate that the carbon detonation at the surface of a neutron star is amultiscale phenomenon. The length scale of liberation of energy is $10^6$ timessmaller than the total reaction length. We show that a multi-resolutionapproach can be used to solve all the reaction lengths. This result will bevery useful in future multi-dimensional simulations. We present alsothermodynamical and composition profiles after the passage of a detonation in apure carbon or mixed carbon-iron layer, in thermodynamical conditions relevantto superbursts in pure helium accretor systems.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The large quantity and high quality of modern radio and infrared lineobservations require efficient modeling techniques to infer physical andchemical parameters such as temperature, density, and molecular abundances. Wepresent a computer program to calculate the intensities of atomic and molecularlines produced in a uniform medium, based on statistical equilibriumcalculations involving collisional and radiative processes and includingradiation from background sources. Optical depth effects are treated with anescape probability method. The program is available on the World Wide Web athttp://www.sron.rug.nl/~vdtak/radex/index.shtml . The program makes use ofmolecular data files maintained in the Leiden Atomic and Molecular Database(LAMDA), which will continue to be improved and expanded. The performance ofthe program is compared with more approximate and with more sophisticatedmethods. An Appendix provides diagnostic plots to estimate physical parametersfrom line intensity ratios of commonly observed molecules. This program shouldform an important tool in analyzing observations from current and future radioand infrared telescopes.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We propose a model of a heterogeneous glass forming liquid and compute thelow-temperature behavior of a tagged molecule moving within it. This modelexhibits stretched-exponential decay of the wavenumber-dependent, selfintermediate scattering function in the limit of long times. At temperaturesclose to the glass transition, where the heterogeneities are much larger inextent than the molecular spacing, the time dependence of the scatteringfunction crosses over from stretched-exponential decay with an index $b=1/2$ atlarge wave numbers to normal, diffusive behavior with $b = 1$ at smallwavenumbers. There is a clear separation between early-stage, cage-breaking$\\beta$ relaxation and late-stage $\\alpha$ relaxation. The spatialrepresentation of the scattering function exhibits an anomalously broadexponential (non-Gaussian) tail for sufficiently large values of the moleculardisplacement at all finite times.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "A detailed study of the geometries that emerge by a gravitating generalizedYang monopole in even dimensions is carried out. In particular, those whichpresent black hole and cosmological horizons. This two-horizon system isthermally unstable. The process of thermalization will drive both horizons tocoalesce. This limit is what is profusely studied in this paper. It is shownthat eventhough coordinate distance shrinks to zero, physical distance doesnot. So, there is some remaining space which geometry has been computed andidentified as a generalized Nariai solution. The thermal properties of this newspacetime are then calculated. Topics, as the elliptical relation between radiiof spheres in the geometry or a discussion about whether a mass-type termshould be present in the line element or not, are also included.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The geometric constructions are elaborated on (semi) Riemannian manifolds andvector bundles provided with nonintegrable distributions defining nonlinearconnection structures induced canonically by metric tensors. Such spaces arecalled nonholonomic manifolds and described by two equivalent linearconnections also induced in unique forms by a metric tensor (the Levi Civitaand the canonical distinguished connection, d-connection). The lifts ofgeometric objects on tangent bundles are performed for certain classes ofd-connections and frame transforms when the Riemann tensor is parametrized byconstant matrix coefficients. For such configurations, the flows ofnon-stretching curves and corresponding bi-Hamilton and solitonic hierarchiesencode information about Ricci flow evolution, Einstein spaces and exactsolutions in gravity and geometric mechanics. The applied methods wereelaborated formally in Finsler geometry and allows us to develop the formalismfor generalized Riemann-Finsler and Lagrange spaces. Nevertheless, allgeometric constructions can be equivalently re-defined for the Levi Civitaconnections and holonomic frames on (semi) Riemannian manifolds.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We extend Hendriks' classification theorem and Turaev's realisation andsplitting theorems for Poincare duality complexes in dimension three to therelative case of Poincare duality pairs. The results for Poincare dualitycomplexes are recovered by restricting the results to the case of Poincareduality pairs with empty boundary. Up to oriented homotopy equivalence,three-dimensional Poincare duality pairs are classified by their fundamentaltriple consisting of the fundamental group system, the orientation characterand the image of the fundamental class under the classifying map. Using thederived module category we provide necessary and sufficient conditions for agiven triple to be realised by a three-dimensional Poincare duality pair. Theresults on classification and realisation yield splitting or decompositiontheorems for three-dimensional Poincare duality pairs, that is, conditionsunder which a given three-dimensional Poincare duality pair decomposes asinterior or boundary connected sum of two three-dimensional Poincare dualitypairs.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We critically examine issues associated with determining the fundamentalproperties of the black hole and the surrounding accretion disk in an X-raybinary based on modeling the disk X-ray continuum of the source. We base ourwork mainly on two XMM-Newton observations of GX 339-4, because they providedhigh-quality data at low energies (below 1 keV) which are critical for reliablymodeling the spectrum of the accretion disk. A key issue examined is thedetermination of the so-called \"color correction factor\", which is oftenempirically introduced to account for the deviation of the local disk spectrumfrom a blackbody (due to electron scattering). This factor cannot bepre-determined theoretically because it may vary with, e.g., mass accretionrate, among a number of important factors. We follow up on an earliersuggestion to estimate the color correction observationally by modeling thedisk spectrum with saturated Compton scattering. We show that the spectra canbe fitted well and the approach yields reasonable values for the colorcorrection factor. For comparison, we have also attempted to fit the spectrawith other models. We show that even the high-soft-state continuum (which isdominated by the disk emission) cannot be satisfactorily fitted bystate-of-the-art disk models. We discuss the implication of the results.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Although there is mounting observational evidence that the cosmic expansionis undergoing a late-time acceleration, the physical mechanism behind such aphenomenon is yet unknown. In this paper, we investigate a holographic darkenergy (HDE) model with interaction between the components of the dark sectorin the light of current cosmological observations. We use both the new\\emph{gold} sample of 182 type Ia supernovae (SNe Ia) and the 192 SNe IaESSENCE data, the baryon acoustic oscillation measurement from the SloanDigital Sky Survey and the shift parameter from the three-year WilkinsonMicrowave Anisotropy Probe data. In agreement with previous results, we showthat these observations suggest a very weak coupling or even a noninteractingHDE. The phantom crossing behavior in the context of these scenarios is alsobriefly discussed.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Mixing is one of the basic functions which automated lab-on-chips require forthe effective management of liquid samples. In this paper we report on theworking principle, design, fabrication and experimental characterization of asoft-lithographed micromixer for microfluidic applications. The deviceeffectively mixes two liquids by means of chaotic advection obtained as animplementation of a Linked Twisted Map (LTM). In this sense it is chaotic. Theliquids are electrokinetically displaced by generating rolls through ACelectroosmosis on co-planar electrodes. The device performance has been testedon dyed DI-water for several voltages, frequencies and flow-rates, displayinggood mixing properties in the range of $10 \\div 100$kHz, at low peak-to-peakvoltages ($\\sim15 \\div 20$ volts). Low voltage supply, small dimensions andpossibility of fabrication via standard lithographic techniques make the devicehighly integrable in lab-on-a-chip platforms.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "This paper is devoted to the analysis of a second order method for recoveringthe \\emph{a priori} unknown shape of an inclusion $\\omega$ inside a body$\\Omega$ from boundary measurement. This inverse problem - known as electricalimpedance tomography - has many important practical applications and hence hasfocussed much attention during the last years. However, to our best knowledge,no work has yet considered a second order approach for this problem. This paperaims to fill that void: we investigate the existence of second order derivativeof the state $u$ with respect to perturbations of the shape of the interface$\\partial\\omega$, then we choose a cost function in order to recover thegeometry of $\\partial \\omega$ and derive the expression of the derivativesneeded to implement the corresponding Newton method. We then investigate thestability of the process and explain why this inverse problem is severelyill-posed by proving the compactness of the Hessian at the global minimizer.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The existence of a clumpy, large-scale filamentary structure is at the basisof the current paradigm of cosmic formation and evolution of clusters. Thestar-formation history of galaxies falling into a cluster is altered as aresult of the environmental stresses. We investigate the relation betweensubstructure and properties of the galaxy population in a 30'x30' regioncentered on the massive merging cluster A2744 at z~0.3. Multi-objectspectroscopy at low resolution and BVR photometry are used to detect thepresence of substructure through a Dressler-Schectman analysis and thephotometric redshift technique, respectively. Galaxies at the same photometricredshift of the cluster are divided into red and blue according to theirdistribution in the B-R vs. R colour-magnitude diagram. We identify twolarge-scale filaments associated with A2744. Along these filaments, theblue-to-red galaxy number ratio increases together with the cluster-centricdistance but peaks slightly beyond the cluster virial radius. The filamentshost a population of bright, large (i.e. more luminous than R* for the mainbody of the cluster and with angular sizes of 13-22 $h_{70}^{-1}$ kpc) bluegalaxies that is hardly found among galaxies lying in a neighbouringlow-density environment at the same redshift of the cluster. These results canbe interpreted as a manifestation of galaxy harassment.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The past two Decadal Surveys in Astronomy and Astrophysics recommended thecompletion of a space-based interferometry mission, known today as SIMPlanetQuest, for its unique ability to detect and characterize nearby rockyplanets (Bahcall 1991, McKee & Taylor 2001), as well as contributions to abroad range of problems in astrophysics. Numerous committees of the NationalResearch Council as well as NASA Roadmaps have similarly highlighted SIM as theone technology that offers detection and characterization of rocky planetsaround nearby stars and which is technically ready. To date, SIM remains theonly program with the capability of detecting and confirming rocky planets inthe habitable zones of nearby solar-type stars. Moreover, SIM measures massesand three-dimensional orbits of habitable planets around nearby stars (within25 pc); these are the only stars for which follow-up by other techniques isfeasible, such as space-based spectroscopy, ground-based interferometry, and ofcourse TPF.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present a hierarchical simulation approach for the dependability analysisand evaluation of a highly available commercial cache-based RAID storagesystem. The archi-tecture is complex and includes several layers ofoverlap-ping error detection and recovery mechanisms. Three ab-straction levelshave been developed to model the cache architecture, cache operations, anderror detection and recovery mechanism. The impact of faults and errorsoc-curring in the cache and in the disks is analyzed at each level of thehierarchy. A simulation submodel is associated with each abstraction level. Themodels have been devel-oped using DEPEND, a simulation-based environment forsystem-level dependability analysis, which provides facili-ties to injectfaults into a functional behavior model, to simulate error detection andrecovery mechanisms, and to evaluate quantitative measures. Several faultmodels are defined for each submodel to simulate cache component failures, diskfailures, transmission errors, and data errors in the cache memory and in thedisks. Some of the parame-ters characterizing fault injection in a givensubmodel cor-respond to probabilities evaluated from the simulation of thelower-level submodel. Based on the proposed method-ology, we evaluate andanalyze 1) the system behavior un-der a real workload and high error rate(focusing on error bursts), 2) the coverage of the error detection mechanismsimplemented in the system and the error latency distribu-tions, and 3) theaccumulation of errors in the cache and in the disks.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Precise photometric measurements of the upcoming space missions allow thesize, mass, and density of satellites of exoplanets to be determined. Here wepresent such an analysis using the photometric transit timing variation($TTV_p$). We examined the light curve effects of both the transiting planetand its satellite. We define the photometric central time of the transit thatis equivalent to the transit of a fixed photocenter. This point orbits thebarycenter, and leads to the photometric transit timing variations. The exactvalue of $TTV_p$ depends on the ratio of the density, the mass, and the size ofthe satellite and the planet. Since two of those parameters are independent, areliable estimation of the density ratio leads to an estimation of the size andthe mass of the exomoon. Upper estimations of the parameters are possible inthe case when an upper limit of $TTV_p$ is known. In case the density ratiocannot be estimated reliably, we propose an approximation with assuming equaldensities. The presented photocenter $TTV_p$ analysis predicts the size of thesatellite better than the mass. We simulated transits of the Earth-Moon systemin front of the Sun. The estimated size and mass of the Moon are 0.020Earth-mass and 0.274 Earth-size if equal densities are assumed. This result iscomparable to the real values within a factor of 2. If we include the realdensity ratio (about 0.6), the results are 0.010 Earth-Mass and 0.253Earth-size, which agree with the real values within 20%.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "A computational model study for complete frequency redistribution linearincoherent two-level atomic radiation trapping in optically dense media usingthe multiple scattering representation is presented. This model study discussat length the influence of the spectral distributions, overall opacity andemission quantum yield to trapping distorted ensemble quantities stressingphysical insight and with a non-specialist audience in mind. Macroscopicreemission yield, lifetime, steady state spectra and spatial distributions arecalculated as a function of intrinsic emission yield, opacity and externalexcitation mode for Doppler, Lorentz and Voigt lineshapes. The work couldconstitute the basis for a final undergraduate or beginning graduate project incomputational physics instruction and implements the analytical developments ofthe previous instalment of this contribution.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We study the influence of cooperative effects such as superradiance andsubradiance, on the scattering properties of dilute atomic gases. We show thatcooperative effects lead to an effective potential between pairs of atoms thatdecays like $1/r$. In the case of superradiance, this potential is attractivefor close enough atoms and can be interpreted as a coherent mesoscopic effect.We consider a model of multiple scattering of a photon among superradiant pairsand calculate the elastic mean free path and the group velocity. We study firstthe case of a scalar wave which allows to obtain and to understand basicfeatures of cooperative effects and multiple scattering. We then turn to thegeneral problem of a vector wave. In both cases, we obtain qualitativelysimilar results and derive, for the case of a scalar wave, analytic expressionsof the elastic mean free path and of the group velocity for an arbitrary (nearresonance) detuning.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The current-voltage (I-V) characteristics of various MgB2 films have beenstudied at different magnetic fields parallel to c-axis. At fields \\mu0Hbetween 0 and 5T, vortex liquid-glass transitions were found in the I-Visotherms. Consistently, the I-V curves measured at different temperatures showa scaling behavior in the framework of quasi-two-dimension (quasi-2D) vortexglass theory. However, at \\mu0 H >= 5T, a finite dissipation was observed downto the lowest temperature here, T=1.7K, and the I-V isotherms did not scale interms of any known scaling law, of any dimensionality. We suggest that this maybe caused by a mixture of \\sigma band vortices and \\pi band quasiparticles.Interestingly, the I-V curves at zero magnetic field can still be scaledaccording to the quasi-2D vortex glass formalism, indicating an equivalenteffect of self-field due to persistent current and applied magnetic field.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present a study of rotation (vsini) and chromospheric activity (Halpha EW)based on an extensive set of high-resolution optical spectra obtained with MIKEon the 6.5m Magellan Clay telescope. Our targets are 74 F-M dwarfs in the youngstellar associations Eta Cha, TW Hydrae, Beta Pic, and Tuc-Hor, spanning agesfrom 6 to 30 Myr. While the Halpha EW for most F and G stars are consistentwith pure photospheric absorption, most K and M stars show chromosphericemission. By comparing Halpha EW in our sample to results in the literature, wesee a clear evolutionary sequence: Chromospheric activity declines steadilyfrom the T Tauri phase to the main sequence. Using activity as an ageindicator, we find a plausible age range for the Tuc-Hor association of 10-40Myr. Between 5 and 30 Myr, we do not see evidence for rotational braking in thetotal sample, thus angular momentum is conserved, in contrast to younger stars.This difference indicates a change in the rotational regulation at 5-10 Myr,possibly because disk braking cannot operate longer than typical disklifetimes, allowing the objects to spin up. The rotation-activity relation isflat in our sample; in contrast to main-sequence stars, there is no linearcorrelation for slow rotators. We argue that this is because young starsgenerate their magnetic fields in a fundamentally different way frommain-sequence stars, and not just the result of a saturated solar-type dynamo.By comparing our rotational velocities with published rotation periods for asubset of stars, we determine ages of 13 (7-20) Myr and 9 (7-17} Myr for theEta Cha and TWA associations, respectively, consistent with previous estimates.Thus we conclude that stellar radii from evolutionary models by Baraffe et al.(1998) are in agreement with the observed radii within +-15%. (abridged)", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "In this series of three papers we present results from a combinedexperimental and theoretical effort to quantitatively describe capacitivelycoupled radio-frequency discharges in oxygen. The particle-in-cell Monte-Carlomodel on which the theoretical description is based will be described in thepresent paper. It treats space charge fields and transport processes on anequal footing with the most important plasma-chemical reactions. For givenexternal voltage and pressure, the model determines the electric potentialwithin the discharge and the distribution functions for electrons, negativelycharged atomic oxygen, and positively charged molecular oxygen. Previously usedscattering and reaction cross section data are critically assessed and in somecases modified. To validate our model, we compare the densities in the bulk ofthe discharge with experimental data and find good agreement, indicating thatessential aspects of an oxygen discharge are captured.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We study a novel configuration for displacement detection consisting of ananomechanical resonator coupled to both, a radio frequency superconductinginterference device (RF SQUID) and to a superconducting stripline resonator. Weemploy an adiabatic approximation and rotating wave approximation and calculatethe displacement sensitivity. We study the performance of such a displacementdetector when the stripline resonator is driven into a region of nonlinearoscillations. In this region the system exhibits noise squeezing in the outputsignal when homodyne detection is employed for readout. We show thatdisplacement sensitivity of the device in this region may exceed the upperbound imposed upon the sensitivity when operating in the linear region. On theother hand, we find that the high displacement sensitivity is accompanied by aslowing down of the response of the system, resulting in a limited bandwidth.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The Kramers' survival probability has been generalized by using nonextensiveformalism. This nonextensive survival probability is studied in detail andassociated Kramers' rate has been calculated in the high and low viscositylimit. It has been showed that the proportionality of nonextensive Kramers'rate to the nonextensive friction term in the high viscosity limit changes toinverse proportionality in the low viscosity limit. It has also been observedthat friction constant of nonextensive processes is of rescaled form of theordinary frictional term. Since the relation between the ordinary rate andnonextensive rate is found out to be linear, the Arrhenius nature of theKramers' rate is preserved. By using experimental results related to COrebinding to myoglobin after photodissociation, we conclude that nonextensivityplays an important role in protein reactions.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present a 127deg x 63deg extinction map of the Anticenter of the Galaxy,based on <J-H> and <H-K> colour excess maps from 2MASS. This 8001 square degreemap with a resolution of 4 arcminutes is provided as online material. Thecolour excess ratio <J-H> / <H-K> is used to determine the power law index ofthe reddening law (\\beta) for individual regions contained in the area (e.g.Orion, Perseus, Taurus, Auriga, Monoceros, Camelopardalis, Cassiopeia). Onaverage we find a dominant value of \\beta=1.8+-0.2 for the individual clouds,in agreement with the canonical value for the interstellar medium. We also showthat there is an internal scatter of \\beta values in these regions, and that insome areas more than one dominant \\beta value is present. This indicates largescale variations in the dust properties. The analysis of the A_V values withinindividual regions shows a change in the slope of the column densitydistribution with distance. This can either be attributed to a change in thegoverning physical processes in molecular clouds on spatial scales of about 1pcor an A_V dilution with distance in our map.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "In this paper we present an upper bound for the decay of correlation for thestationary stochastic process associated with the Entropy Penalized Method. Let$L(x, v):\\Tt^n\\times\\Rr^n\\to \\Rr$ be a Lagrangian of the form  L(x,v) = {1/2}|v|^2 - U(x) + < P, v>.  For each value of $\\epsilon $ and $h$, consider the operator  \\Gg[\\phi](x):= -\\epsilon h {ln}[\\int_{\\re^N} e^{-\\frac{hL(x,v)+\\phi(x+hv)}{\\epsilon h}}dv], as well as the reversed operator\\bar \\Gg[\\phi](x):= -\\epsilon h {ln}[\\int_{\\re^N}e^{-\\frac{hL(x+hv,-v)+\\phi(x+hv)}{\\epsilon h}}dv], both acting on continuousfunctions $\\phi:\\Tt^n\\to \\Rr$. Denote by $\\phi_{\\epsilon,h} $ the solution of$\\Gg[\\phi_{\\epsilon,h}]=\\phi_{\\epsilon,h}+\\lambda_{\\epsilon,h}$, and by $\\bar\\phi_{\\epsilon,h} $ the solution of $\\bar \\Gg[\\phi_{\\epsilon,h}]=\\bar\\phi_{\\epsilon,h}+\\lambda_{\\epsilon,h}$. In order to analyze the decay ofcorrelation for this process we show that the operator $ {\\cal L} (\\phi) (x) =\\int e^{- \\frac{h L (x,v)}{\\epsilon}} \\phi(x+h v) d v,$ has a maximaleigenvalue isolated from the rest of the spectrum.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We report new magnetic field measurements for 14 classical T Tauri stars(CTTSs). We combine these data with one previous field determination in orderto compare our observed field strengths with the field strengths predicted bymagnetospheric accretion models. We use literature data on the stellar mass,radius, rotation period, and disk accretion rate to predict the field strengththat should be present on each of our stars according to these magnetosphericaccretion models. We show that our measured field values do not correlate withthe field strengths predicted by simple magnetospheric accretion theory. Wealso use our field strength measurements and literature X-ray luminosity datato test a recent relationship expressing X-ray luminosity as a function ofsurface magnetic flux derived from various solar feature and main sequence starmeasurements. We find that the T Tauri stars we have observed have weaker thanexpected X-ray emission by over an order of magnitude on average using thisrelationship. We suggest the cause for this is actually a result of the verystrong fields on these stars which decreases the efficiency with which gasmotions in the photosphere can tangle magnetic flux tubes in the corona.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Higher-Order Fixpoint Logic (HFL) is a hybrid of the simply typed\\lambda-calculus and the modal \\lambda-calculus. This makes it a highlyexpressive temporal logic that is capable of expressing various interestingcorrectness properties of programs that are not expressible in the modal\\lambda-calculus.  This paper provides complexity results for its model checking problem. Inparticular we consider those fragments of HFL built by using only types ofbounded order k and arity m. We establish k-fold exponential time completenessfor model checking each such fragment. For the upper bound we use fixpointelimination to obtain reachability games that are singly-exponential in thesize of the formula and k-fold exponential in the size of the underlyingtransition system. These games can be solved in deterministic linear time. As asimple consequence, we obtain an exponential time upper bound on the expressioncomplexity of each such fragment.  The lower bound is established by a reduction from the word problem foralternating (k-1)-fold exponential space bounded Turing Machines. Since thereare fixed machines of that type whose word problems are already hard withrespect to k-fold exponential time, we obtain, as a corollary, k-foldexponential time completeness for the data complexity of our fragments of HFL,provided m exceeds 3. This also yields a hierarchy result in expressive power.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Owing to their distinct properties, carbon nanotubes (CNTs) have emerged aspromising candidate for field emission devices. It has been foundexperimentally that the results related to the field emission performance showvariability. The design of an efficient field emitting device requires theanalysis of the variabilities with a systematic and multiphysics based modelingapproach. In this paper, we develop a model of randomly oriented CNTs in a thinfilm by coupling the field emission phenomena, the electron-phonon transportand the mechanics of single isolated CNT. A computational scheme is developedby which the states of CNTs are updated in time incremental manner. The devicecurrent is calculated by using Fowler-Nordheim equation for field emission tostudy the performance at the device scale.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We differentiate between the metal enrichment of the gas in virializedminihalos and that of the intergalactic medium at high redshift, pertinent tocosmological reionization, with the initial expectation that gas in the highdensity regions within formed dark matter halos may be more robust thusresistant to mixing with lower density intergalactic medium. Using detailedhydrodynamic simulations of gas clouds in minihalos subject to destructiveprocesses associated with the encompassing intergalactic shocks carryingmetal-enriched gas, we find, as an example, that, for realistic shocks ofvelocities of 10-100km/s, more than (90%,65%) of the high density gas withrho>500 rhob inside a minihalo virialized at z=10 of mass (10^7,10^6)Msunremains at a metallicity lower than 3% of that of the intergalactic medium byredshift z=6. It may be expected that the high density gas in minihalos becomesfuel for subsequent star formation, when they are incorporated into largerhalos where efficient atomic cooling can induce gas condensation hence starformation. Since minihalos virialize at high redshift when the universe is notexpected to have been significantly reionized, the implication is that gas invirialized minihalos may provide an abundant reservoir of primordial gas topossibly allow for the formation of Population-III metal-free stars to extendto much lower redshift than otherwise expected based on the enrichment ofintergalactic medium.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The rotor-router model is a deterministic analogue of random walk. It can beused to define a deterministic growth model analogous to internal DLA. We showthat the set of occupied sites for this model on an infinite regular tree is aperfect ball whenever it can be, provided the initial rotor configuration isacyclic (that is, no two neighboring vertices have rotors pointing to oneanother). This is proved by defining the rotor-router group of a graph, whichwe show is isomorphic to the sandpile group. We also address the question ofrecurrence and transience: We give two rotor configurations on the infiniteternary tree, one for which chips exactly alternate escaping to infinity withreturning to the origin, and one for which every chip returns to the origin.Further, we characterize the possible \"escape sequences\" for the ternary tree,that is, binary words a_1 ... a_n for which there exists a rotor configurationso that the k-th chip escapes to infinity if and only if a_k=1.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We have performed self-consistent 2.5-dimensional nonsteady MHD numericalsimulations of jet formation as long as possible, including the dynamics ofaccretion disks. Although the previous nonsteady MHD simulations forastrophysical jets revealed that the characteristics of nonsteady jets aresimilar to those of steady jets, the calculation time of these simulations isvery short compared with the time scale of observed jets. Thus we haveinvestigated long term evolutions of mass accretion rate, mass outflow rate,jet velocity, and various energy flux. We found that the ejection of jet isquasi-periodic. The period of the ejection is related to the time needed forthe initial magnetic filed to be twisted to generate toroidal filed. We compareour results with both the steady state theory and previous 2.5-dimensionalnonsteady MHD simulations.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "In this two-part paper, we consider the multiantenna multihop relay channelsin which the source signal arrives at the destination through N independentrelaying hops in series. The main concern of this work is to design relayingstrategies that utilize efficiently the relays in such a way that the diversityis maximized. In part I, we focus on the amplify-and-forward (AF) strategy withwhich the relays simply scale the received signal and retransmit it. Morespecifically, we characterize the diversity-multiplexing tradeoff (DMT) of theAF scheme in a general multihop channel with arbitrary number of antennas andarbitrary number of hops. The DMT is in closed-form expression as a function ofthe number of antennas at each node. First, we provide some basic results onthe DMT of the general Rayleigh product channels. It turns out that theseresults have very simple and intuitive interpretation. Then, the results areapplied to the AF multihop channels which is shown to be equivalent to theRayleigh product channel, in the DMT sense. Finally, the project-and-forward(PF) scheme, a variant of the AF scheme, is proposed. We show that the PFscheme has the same DMT as the AF scheme, while the PF can have significantpower gain over the AF scheme in some cases. In part II, we will derive theupper bound on the diversity of the multihop channels and show that it can beachieved by partitioning the multihop channel into AF subchannels.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Gravitational waves from the inspiral and coalescence of supermassiveblack-hole (SMBH) binaries with masses ~10^6 Msun are likely to be among thestrongest sources for the Laser Interferometer Space Antenna (LISA). Wedescribe a three-stage data-analysis pipeline designed to search for andmeasure the parameters of SMBH binaries in LISA data. The first stage uses atime-frequency track-search method to search for inspiral signals and provide acoarse estimate of the black-hole masses m_1, m_2 and of the coalescence timeof the binary t_c. The second stage uses a sequence of matched-filter templatebanks, seeded by the first stage, to improve the measurement accuracy of themasses and coalescence time. Finally, a Markov Chain Monte Carlo search is usedto estimate all nine physical parameters of the binary. Using results from thesecond stage substantially shortens the Markov Chain burn-in time and allows usto determine the number of SMBH-binary signals in the data before startingparameter estimation. We demonstrate our analysis pipeline using simulated datafrom the first LISA Mock Data Challenge. We discuss our plan for improving thispipeline and the challenges that will be faced in real LISA data analysis.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We replace the ice Ansatz on matrix solutions of the Yang-Baxter equation bya weaker condition which we call \"rime\". Rime solutions include the standardDrinfeld-Jimbo R-matrix. Solutions of the Yang--Baxter equation within the rimeAnsatz which are maximally different from the standard one we call \"strictrime\". A strict rime non-unitary solution is parameterized by a projectivevector. We show that this solution transforms to the Cremmer-Gervais R-matrixby a change of basis with a matrix containing symmetric functions in thecomponents of the parameterizing vector. A strict unitary solution (the rimeAnsatz is well adapted for taking a unitary limit) is shown to be equivalent toa quantization of a classical \"boundary\" r-matrix of Gerstenhaber andGiaquinto. We analyze the structure of the elementary rime blocks and find, asa by-product, that all non-standard R-matrices of GL(1|1)-type can be uniformlydescribed in a rime form.  We discuss then connections of the classical rime solutions with the Bezoutoperators. The Bezout operators satisfy the (non-)homogeneous associativeclassical Yang--Baxter equation which is related to the Rota-Baxter operators.  We classify the rime Poisson brackets: they form a 3-dimensional pencil. Anormal form of each individual member of the pencil depends on the discriminantof a certain quadratic polynomial. We also classify orderable quadratic rimeassociative algebras.  For the standard Drinfeld-Jimbo solution, there is a choice of themultiparameters, for which it can be non-trivially rimed. However, not everyBelavin-Drinfeld triple admits a choice of the multiparameters for which it canbe rimed. We give a minimal example.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We perform a comprehensive analysis of the Minimal Supersymmetric StandardModel (MSSM) in the scenario where the scalar partners of the fermions and theHiggs particles (except for the Standard-Model-like one) are assumed to be veryheavy and are removed from the low-energy spectrum. We first summarize ourdetermination of the mass spectrum, in which we include the one-loop radiativecorrections and resum to all orders the leading logarithms of the large scalarmasses, and describe the implementation of these features in the FORTRAN codeSuSpect which calculates the masses and couplings of the MSSM particles. Wethen study in detail the phenomenology of the model in scenarios where thegaugino mass parameters are non-universal at the GUT scale, which leads to veryinteresting features that are not present in the widely studied case ofuniversal gaugino mass parameters. We discuss the constraints from collidersearches and high-precision measurements, the cosmological constraints on therelic abundance of the neutralino candidate for the Dark Matter in the Universe- where new and interesting channels for neutralino annihilation appear - andthe gluino lifetime. We then analyze, in the case of non-universal gauginomasses, the decays of the Higgs boson (in particular decays into andcontributions of SUSY particles), of charginos and neutralinos (in particulardecays into Higgs bosons and photons) and of gluinos, and highlight thedifferences from the case of universal gaugino masses.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present a search for the near infrared spectroscopic signature of theclose orbiting extrasolar giant planet HD 75289b. We obtained ~230 spectra inthe wavelength range 2.18 - 2.19 microns using the Phoenix spectrograph atGemini South. By considering the direct spectrum, derived from irradiated modelatmospheres, we search for the absorption profile signature present in thecombined star and planet light. Since the planetary spectrum is separated fromthe stellar spectrum at most phases, we apply a phase dependent orbital modeland tomographic techniques to search for absorption signatures.  Because the absorption signature lies buried in the noise of a singleexposure we apply a multiline deconvolution to the spectral lines available inorder to boost the effective S/N ratio of the data. The wavelength coverage of80 angstroms is expected to contain ~100 planetary lines, enabling a mean linewith S/N ratio of ~800 to be achieved after deconvolution. We are neverthelessunable to detect the presence of the planet in the data and carry out furthersimulations to show that broader wavelength coverage should enable a planetlike HD 75289b to be detected with 99.9 per cent (4 sigma) confidence. Weinvestigate the sensitivity of our method and estimate detection tolerances formismatches between observed and model planetary atmospheres.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We characterize the dynamical behavior of continuous-time, Markovian quantumsystems with respect to a subsystem of interest. Markovian dynamics describes awide class of open quantum systems of relevance to quantum informationprocessing, subsystem encodings offering a general pathway to faithfullyrepresent quantum information. We provide explicit linear-algebraiccharacterizations of the notion of invariant and noiseless subsystem forMarkovian master equations, under different robustness assumptions formodel-parameter and initial-state variations. The stronger concept of anattractive quantum subsystem is introduced, and sufficient existence conditionsare identified based on Lyapunov's stability techniques. As a main controlapplication, we address the potential of output-feedback Markovian controlstrategies for quantum pure state-stabilization and noiseless-subspacegeneration. In particular, explicit results for the synthesis of stabilizingsemigroups and noiseless subspaces in finite-dimensional Markovian systems areobtained.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The interference channel with degraded message sets (IC-DMS) refers to acommunication model in which two senders attempt to communicate with theirrespective receivers simultaneously through a common medium, and one of thesenders has complete and a priori (non-causal) knowledge about the messagebeing transmitted by the other. A coding scheme that collectively hasadvantages of cooperative coding, collaborative coding, and dirty paper coding,is developed for such a channel. With resorting to this coding scheme,achievable rate regions of the IC-DMS in both discrete memoryless and Gaussiancases are derived, which, in general, include several previously known rateregions. Numerical examples for the Gaussian case demonstrate that in thehigh-interference-gain regime, the derived achievable rate regions offerconsiderable improvements over these existing results.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We follow the changes in the structure of the accretion disk of the dwarfnova V2051 Oph along two separate outbursts in order to investigate the causesof its recurrent outbursts. We apply eclipse mapping techniques to a set oflight curves covering a normal (July 2000) and a low-amplitude (August 2002)outburst to derive maps of the disk surface brightness distribution atdifferent phases along the outburst cycles. The sequence of eclipse maps of the2000 July outburst reveal that the disk shrinks at outburst onset while anuneclipsed component of 13 per cent of the total light develops. The derivedradial intensity distributions suggest the presence of an outward-movingheating wave during rise and of an inward-moving cooling wave during decline.The inferred speed of the outward-moving heating wave is ~ 1.6 km/s, while thespeed of the cooling wave is a fraction of that. A comparison of the measuredcooling wave velocity on consecutive nights indicates that the cooling waveaccelerates as it travels towards disk center, in contradiction with theprediction of the disk instability model. From the inferred speed of theheating wave we derive a viscosity parameter alpha_{hot} ~ 0.13, comparable tothe measured viscosity parameter in quiescence. The 2002 August outburst hadlower amplitude (\\Delta B ~ 0.8 mag) and the disk at outburst maximum wassmaller than on 2000 July. For an assumed distance of 92 pc, we find that alongboth outbursts the disk brightness temperatures remain below the minimumexpected according to the disk instability model. The results suggest that theoutbursts of V2051 Oph are caused by bursts of increased mass transfer from themass-donor star.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We estimate the spin relaxation rate due to spin-orbit coupling and acousticphonon scattering in weakly-confined quantum dots with up to five interactingelectrons. The Full Configuration Interaction approach is used to account forthe inter-electron repulsion, and Rashba and Dresselhaus spin-orbit couplingsare exactly diagonalized. We show that electron-electron interaction stronglyaffects spin-orbit admixture in the sample. Consequently, relaxation ratesstrongly depend on the number of carriers confined in the dot. We identify themechanisms which may lead to improved spin stability in few electron (>2)quantum dots as compared to the usual one and two electron devices. Finally, wediscuss recent experiments on triplet-singlet transitions in GaAs dots subjectto external magnetic fields. Our simulations are in good agreement with theexperimental findings, and support the interpretation of the observed spinrelaxation as being due to spin-orbit coupling assisted by acoustic phononemission.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present multi-wavelength optical and infrared photometry of 170 previouslyknown low mass stars and brown dwarfs of the 5 Myr Collinder 69 cluster (LambdaOrionis). The new photometry supports cluster membership for most of them, withless than 15% of the previous candidates identified as probable non-members.The near infrared photometry allows us to identify stars with IR excesses, andwe find that the Class II population is very large, around 25% for stars (inthe spectral range M0 - M6.5) and 40% for brown dwarfs, down to 0.04 Msun,despite the fact that the H(alpha) equivalent width is low for a significantfraction of them. In addition, there are a number of substellar objects,classified as Class III, that have optically thin disks. The Class II membersare distributed in an inhomogeneous way, lying preferentially in a filamentrunning toward the south-east. The IR excesses for the Collinder 69 membersrange from pure Class II (flat or nearly flat spectra longward of 1 micron), totransition disks with no near-IR excess but excesses beginning within the IRACwavelength range, to two stars with excess only detected at 24 micron.Collinder 69 thus appears to be at an age where it provides a naturallaboratory for the study of primordial disks and their dissipation.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We study the thermal interaction between two nearby thin metallic wires, atfinite temperature. It is shown that the Johnson currents in the wires giverise, via inductive coupling, to a repulsive force between them. This thermalinteraction exhibits all the puzzling features found recently in the thermalCasimir effect for lossy metallic plates, suggesting that the physical originof the difficulties encountered in the Casimir problem resides in the inductivecoupling between the Johnson currents inside the plates. We show that in oursimple model all puzzles are resolved if account is taken of capacitive effectsassociated with the end points of the wires. Our findings suggest thatcapacitive finite-size effects may play an important role in the resolution ofthe analogous problems met in the thermal Casimir effect.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We introduce VErsatile SPectral Analysis (VESPA): a new method which aims torecover robust star formation and metallicity histories from galactic spectra.VESPA uses the full spectral range to construct a galaxy history from syntheticmodels. We investigate the use of an adaptative parametrization grid to recoverreliable star formation histories on a galaxy-by-galaxy basis. Our goal isrobustness as opposed to high resolution histories, and the method is designedto return high time resolution only where the data demand it. In this paper wedetail the method and we present our findings when we apply VESPA to syntheticand real Sloan Digital Sky Survey (SDSS) spectroscopic data. We show that thenumber of parameters that can be recovered from a spectrum depends strongly onthe signal-to-noise, wavelength coverage and presence or absence of a youngpopulation. For a typical SDSS sample of galaxies, we can normally recoverbetween 2 to 5 stellar populations. We find very good agreement between VESPAand our previous analysis of the SDSS sample with MOPED.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The magnetoelectric behavior of BiFeO$_3$ has been explored on the basis ofaccurate density functional calculations. The structural, electronic, magnetic,and ferroelectric properties of BiFeO$_3$ are predicted correctly withoutincluding strong correlation effect in the calculation. Moreover, theexperimentally-observed elongation of cubic perovskite-like lattice along the[111] direction is correctly reproduced. At high pressure we predicted apressure-induced structural transition and the total energy calculations atexpanded lattice show two lower energy ferroelectric phases, closer in energyto the ground state phase. Band-structure calculations show that BiFeO$_3$ willbe an insulator in A- and G-type antiferromagnetic phases and a metal in othermagnetic configurations. Chemical bonding in BiFeO$_3$ has been analyzed usingvarious tools and electron localization function analysis shows thatstereochemically active lone-pair electrons at the Bi sites are responsible fordisplacements of the Bi atoms from the centro-symmetric to thenoncentrosymmetric structure and hence the ferroelectricity. A largeferroelectric polarization (88.7 $\\mu$C/cm$^{2}$) is predicted in accordancewith recent experimental findings. The net polarization is found to mainly ($>$98%) originate from Bi atoms. Moreover the large scatter in experimentallyreported polarization values is due to the large anisotropy in the spontaneouspolarization.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Previously, we have identified the cytoplasmic zinc metalloproteaseinsulin-degrading enzyme(IDE) in human tissues by an immunohistochemical methodinvolving no antigen retrieval (AR) by pressure cooking to avoid artifacts byendogenous biotin exposure and a detection kit based on the labeledstreptavidin biotin (LSAB) method. Thereby, we also employed 3% hydrogenperoxide(H2O2) for the inhibition of endogenous peroxidase activity andincubated the tissue sections with the biotinylated secondary antibody at roomtemperature (RT). We now add the immunohistochemical details that had led us tothis optimized procedure as they also bear a more general relevance whendemonstrating intracellular tissue antigens. Our most important result is thatendogenous peroxidase inhibition by 0.3% H2O2 coincided with an apparentlypositive IDE staining in an investigated breast cancer specimen whereascombining a block by 3% H2O2 with an incubation of the biotinylated secondaryantibody at RT, yet not at 37 degrees Celsius, revealed this specimen as almostentirely IDE-negative. Our present data caution against three differentimmunohistochemical pitfalls that might cause falsely positive results andartifacts when using an LSAB- and peroxidase-based detection method: pressurecooking for AR, insufficient quenching of endogenous peroxidases and heating oftissue sections while incubating with biotinylated secondary antibodies.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present a local interpretation of what is usually considered to be anonlocal de Broglie-Bohm trajectory prescription for an entangled singlet stateof massive particles. After reviewing various meanings of the term``nonlocal'', we show that by using appropriately retarded wavefunctions (i.e.,the locality loophole) this local model can violate Bell's inequality, withoutmaking any appeal to detector inefficiencies.  We analyze a possible experimental configuration appropriate to massivetwo-particle singlet wavefunctions and find that as long as the particles arenot ultra-relativistic, a locality loophole exists and Dirac wave(s) canpropagate from Alice or Bob's changing magnetic field, through space, to theother detector, arriving before the particle and thereby allowing a localinterpretation to the 2-particle de Broglie-Bohm trajectories.  We also propose a physical effect due to changing magnetic fields in aStern-Gerlach EPR setup that will throw away events and create a detectorloophole in otherwise perfectly efficient detectors, an effect that is onlysignificant for near-luminal particles that might otherwise close the localityloophole.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Aims: In the context of space interferometry missions devoted to the searchof exo-Earths, this paper investigates the capabilities of new single modeconductive waveguides at providing modal filtering in an infrared andmonochromatic nulling experiment; Methods: A Michelson laser interferometerwith a co-axial beam combination scheme at 10.6 microns is used. Afterintroducing a Pi phase shift using a translating mirror, dynamic and staticmeasurements of the nulling ratio are performed in the two cases where modalfiltering is implemented and suppressed. No additional active control of thewavefront errors is involved. Results: We achieve on average a statisticalnulling ratio of 2.5e-4 with a 1-sigma upper limit of 6e-4, while a best nullof 5.6e-5 is obtained in static mode. At the moment, the impact of externalvibrations limits our ability to maintain the null to 10 to 20 seconds.;Conclusions: A positive effect of SM conductive waveguide on modal filteringhas been observed in this study. Further improvement of the null should bepossible with proper mechanical isolation of the setup.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We have performed a simulation study of Langmuir turbulence in the Earth'sionosphere by means of a Zakharov model with parameters relevant for the Flayer. The model includes dissipative terms to model collisions and Landaudamping of the electrons and ions, and a linear density profile, which modelsthe ionospheric plasma inhomogeneity whose length scale is of the order 10--100km. The injection of energy into the system is modeled by a constant sourceterm in the Zakharov equation. Langmuir turbulence is excited ``on-demand'' incontrolled ionospheric modification experiments where the energy is provided byan HF radio beam injected into the overhead ionospheric plasma. The ensuingturbulence can be studied with radars and in the form of secondary radiationrecorded by ground-based receivers. We have analyzed spectral signatures of theturbulence for different sets of parameters and different altitudes relative tothe turning point of the linear Langmuir mode where the Langmuir frequencyequals the local plasma frequency. By a parametric analysis, we have derived asimple scaling law, which links the spectral width of the turbulent frequencyspectrum to the physical parameters in the ionosphere. The scaling law providesa quantitative relation between the physical parameters (temperatures, electronnumber density, ionospheric length scale, etc.) and the observed frequencyspectrum. This law may be useful for interpreting experimental results.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Parity doubling in excited hadrons is reviewed. Parity degeneracy in hadronswas first experimentally observed 40 years ago. Recently new experimental dataon light mesons caused much excitement and renewed interest to the phenomenon,which still remains to be enigmatic. The present retrospective review is anattempt to trace the history of parity doubling phenomenon, thus providing akind of introduction to the subject. We begin with early approaches of 1960s(Regge theory and dynamical symmetries) and end up with the latest trends(manifestations of broader degeneracies and AdS/QCD). We show the evolution ofvarious ideas about parity doubling. The experimental evidence for thisphenomenon is scrutinized in the non-strange sector. Some experiments of 1960sdevoted to the search for missing non-strange bosons are re-examined and it isargued that results of these experiments are encouraging from the modernperspective.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Aims: We aim at estimating the spectral energy distributions (SEDs) and thephysical parameters related to the black holes harbored in eight highX-ray-to-optical (F_X/F_R>10) obscured quasars at z>0.9 selected in the 2--10keV band from the HELLAS2XMM survey.  Methods: We use IRAC and MIPS 24 micron observations, along with optical andKs-band photometry, to obtain the SEDs of the sources. The observed SEDs aremodeled using a combination of an elliptical template and torus emission (usingthe phenomenological templates of Silva et al. 2004) for six sources associatedwith passive galaxies; for two point-like sources, the empirical SEDs of redquasars are adopted. The bolometric luminosities and the M_BH-L_K relation areused to provide an estimate of the masses and Eddington ratios of the blackholes residing in these AGN.  Results: All of our sources are detected in the IRAC and MIPS (at 24 micron)bands. The SED modeling described above is in good agreement with the observednear- and mid-infrared data. The derived bolometric luminosities are in therange ~10^45-10^47 erg s^-1, and the median 2--10 keV bolometric correction is~25, consistent with the widely adopted value derived by Elvis et al. (1994).For the objects with elliptical-like profiles in the K_s band, we derive highstellar masses (0.8-6.2)X10^11 Mo, black hole masses in the range(0.2-2.5)X10^9 Mo, and Eddington ratios L/L_Edd<0.1, suggesting a low-accretionphase.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "To examine the evolution of giant molecular clouds in the stream of a hotplasma we performed two-dimensional hydrodynamical simulations that take fullaccount of self-gravity, heating and cooling effects and heat conduction byelectrons. We use the thermal conductivity of a fully ionized hydrogen plasmaproposed by Spitzer and a saturated heat flux according to Cowie & McKee inregions where the mean free path of the electrons is large compared to thetemperature scaleheight. Significant structural and evolutionary differencesoccur between simulations with and without heat conduction. Dense clouds inpure dynamical models experience dynamical destruction by Kelvin-Helmholtz (KH)instability. In static models heat conduction leads to evaporation of suchclouds. Heat conduction acting on clouds in a gas stream smooths out steeptemperature and density gradients at the edge of the cloud because theconduction timescale is shorter than the cooling timescale. This diminishes thevelocity gradient between the streaming plasma and the cloud, so that thetimescale for the onset of KH instabilities increases, and the surface of thecloud becomes less susceptible to KH instabilities. The stabilisation effect ofheat conduction against KH instability is more pronounced for smaller and lessmassive clouds. As in the static case more realistic cloud conditions allowheat conduction to transfer hot material onto the cloud's surface and to mixthe accreted gas deeper into the cloud.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We study resonances of multidimensional chaotic map dynamics. We use thecalculus of variations to determine the additive forcing function that inducesthe largest response, that is, the greatest deviation from the unperturbeddynamics. We include the additional constraint that only select degrees offreedom be forced, corresponding to a very general class of problems in whichnot all of the degrees of freedom in an experimental system are accessible toforcing. We find that certain Lagrange multipliers take on a fundamentalphysical role as the efficiency of the forcing function and the effectiveforcing experienced by the degrees of freedom which are not forced directly.Furthermore, we find that the product of the displacement of nearbytrajectories and the effective total forcing function is a conserved quantity.We demonstrate the efficacy of this methodology with several examples.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The magnetic and thermodynamic properties of spin-1/2 Heisenberg diamondchains are investigated in three different cases: (a) J1, J2, J3>0(frustrated); (b) J1, J3<0, J2>0 (frustrated); and (c) J1, J2>0, J3<0(non-frustrated). The density matrix renormalization group (DMRG) technique isinvoked to study the properties of the system in the ground state, while thetransfer matrix renormalization group (TMRG) technique is applied to explorethe thermodynamic properties. The local magnetic moments, spin correlationfunctions, and static structure factors are discussed in the ground state forthe three cases. It is shown that the static structure factor S(q) shows peaksat wavevectors $q=a\\pi /3$ (a=0,1,2,3,4,5) for different couplings in a zeromagnetic field, which, however in the magnetic fields where the magnetizationplateau with m=1/6 pertains, exhibits the peaks only at q=0, $2\\pi /3$ and$4\\pi /3$, which are found to be couplings-independent. The DMRG results of thezero-field static structure factor can be nicely fitted by a linearsuperposition of six modes, where two fitting equations are proposed. It isobserved that the six modes are closely related to the low-lying excitations ofthe system. At finite temperatures, the double-peak structures of thesusceptibility and specific heat against temperature are obtained, where thepeak positions and heights are found to depend on the competition of thecouplings. It is also uncovered that the XXZ anisotropy of F and AF couplingsleads the system of case (c) to display quite different behaviors. In addition,the experimental data of the susceptibility, specific heat and magnetizationfor the compound Cu$_{3}$(CO$_{3}$)$_{2}$(OH)$_{2}$ are fairly compared withour TMRG results.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Motivation: Profile hidden Markov Models (pHMMs) are a popular and veryuseful tool in the detection of the remote homologue protein families.Unfortunately, their performance is not always satisfactory when proteins arein the 'twilight zone'. We present HMMER-STRUCT, a model construction algorithmand tool that tries to improve pHMM performance by using structural informationwhile training pHMMs. As a first step, HMMER-STRUCT constructs a set of pHMMs.Each pHMM is constructed by weighting each residue in an aligned proteinaccording to a specific structural property of the residue. Properties usedwere primary, secondary and tertiary structures, accessibility and packing.HMMER-STRUCT then prioritizes the results by voting. Results: We used the SCOPdatabase to perform our experiments. Throughout, we apply leave-one-family-outcross-validation over protein superfamilies. First, we used the MAMMOTH-multstructural aligner to align the training set proteins. Then, we performed twosets of experiments. In a first experiment, we compared structure weightedmodels against standard pHMMs and against each other. In a second experiment,we compared the voting model against individual pHMMs. We compare methodperformance through ROC curves and through Precision/Recall curves, and assesssignificance through the paired two tailed t-test. Our results show significantperformance improvements of all structurally weighted models over defaultHMMER, and a significant improvement in sensitivity of the combined models overboth the original model and the structurally weighted models.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "I review the status of science with wide field surveys. For many decadessurveys have been the backbone of astronomy, and the main engine of discovery,as we have mapped the sky at every possible wavelength. Surveys are anefficient use of resources. They are important as a fundamental resource; tomap intrinsically large structures; to gain the necessary statistics to addresssome problems; and to find very rare objects. I summarise major recent widefield surveys - 2MASS, SDSS, 2dfGRS, and UKIDSS - and look at examples of theexciting science they have produced, covering the structure of the Milky Way,the measurement of cosmological parameters, the creation of a new fieldstudying substellar objects, and the ionisation history of the Universe. I thenlook briefly at upcoming projects in the optical-IR survey arena - VISTA,PanSTARRS, WISE, and LSST. Finally I ask, now we have opened up essentially allwavelength windows, whether the exploration of survey discovery space is ended.I examine other possible axes of discovery space, and find them mostly to betoo expensive to explore or otherwise unfruitful, with two exceptions : thefirst is the time axis, which we have only just begun to explore properly; andthe second is the possibility of neutrino astrophysics.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The nonadiabatic Heisenberg model (NHM) proposed as an extension of theHeisenberg model makes a contribution to the eigenstate problem ofsuperconductivity. The Hamiltonian H^n derived within this group-theoreticalmodel has superconducting eigenstates if and only if the considered materialpossesses a narrow, roughly half-filled \"superconducting\" energy band ofspecial symmetry in its band structure. This paper shows that thehigh-temperature superconductor YBa_2Cu_3O_7 possesses such a superconductingband. This new result together with previous observations about othersuperconductors and non-superconductors corroborates the theoretical evidencewithin the NHM that stable superconducting states are connected withsuperconducting bands. It is proposed that the type of superconductivity, i.e.,whether the material is a conventional low-T_c or a high-T_c superconductor, isdetermined by the energetically lowest boson excitations that carry the crystalspin 1*hbar and are sufficiently stable to transport this crystal spin-angularmomentum through the crystal. This mechanism provides the electron-phononmechanism that enters the BCS theory in conventional superconductors.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Inclusive dijet and trijet production in deep inelastic $ep$ scattering hasbeen measured for $10<Q^2<100$ GeV$^2$ and low Bjorken $x$, $10^{-4}<x_{\\rmBj}<10^{-2}$. The data were taken at the HERA $ep$ collider with centre-of-massenergy $\\sqrt{s} = 318 \\gev$ using the ZEUS detector and correspond to anintegrated luminosity of $82 {\\rm pb}^{-1}$. Jets were identified in thehadronic centre-of-mass (HCM) frame using the $k_{T}$ cluster algorithm in thelongitudinally invariant inclusive mode. Measurements of dijet and trijetdifferential cross sections are presented as functions of $Q^2$, $x_{\\rm Bj}$,jet transverse energy, and jet pseudorapidity. As a further examination oflow-$x_{\\rm Bj}$ dynamics, multi-differential cross sections as functions ofthe jet correlations in transverse momenta, azimuthal angles, andpseudorapidity are also presented. Calculations at $\\mathcal{O}(\\alpha_{s}^3)$generally describe the trijet data well and improve the description of thedijet data compared to the calculation at $\\mathcal{O}(\\alpha_{s}^2)$.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We study conditions for the deterministic transformation$\\ket{\\psi}\\longrightarrow\\ket{\\phi}$ of a bipartite entangled state by aseparable operation. If the separable operation is a local operation withclassical communication (LOCC), Nielsen's majorization theorem providesnecessary and sufficient conditions. For the general case we derive a necessarycondition in terms of products of Schmidt coefficients, which is equivalent tothe Nielsen condition when either of the two factor spaces is of dimension 2,but is otherwise weaker. One implication is that no separable operation canreverse a deterministic map produced by another separable operation, if oneexcludes the case where the Schmidt coefficients of $\\ket{\\psi}$ and are thesame as those of $\\ket{\\phi}$. The question of sufficient conditions in thegeneral separable case remains open. When the Schmidt coefficients of$\\ket{\\psi}$ are the same as those of $\\ket{\\phi}$, we show that the Krausoperators of the separable transformation restricted to the supports of$\\ket{\\psi}$ on the factor spaces are proportional to unitaries. When thatproportionality holds and the factor spaces have equal dimension, we findconditions for the deterministic transformation of a collection of several fullSchmidt rank pure states $\\ket{\\psi_j}$ to pure states $\\ket{\\phi_j}$.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The dominant background for observations of gamma-rays in the energy regionabove 50 GeV with Imaging Atmospheric Cherenkov telescopes are cosmic-rayevents. The images of most of the cosmic ray showers look significantlydifferent from those of gamma-rays and are therefore easily discriminated.However, a small fraction of events seems to be indistinguishable fromgamma-rays. This constitutes an irreducible background to the observation ofhigh-energy gamma-ray sources, and limits the sensitivity achievable with agiven instrument. Here, a Monte Carlo study of gamma-like cosmic-ray events ispresented. The nature of gamma-like cosmic-ray events, the shower particlesthat are responsible for the gamma-like appearance, and the dependence of theseresults on the choice of the hadronic interaction model are investigated. Mostof the gamma-like cosmic ray events are characterised by the production ofhigh-energy pi0's early in the shower development which dump most of the showerenergy into electromagnetic sub-showers. Also Cherenkov light from single muonscan mimic gamma-rays in close-by pairs of telescopes. Differences of up to 25%in the collection area for gamma-like proton showers between QGSJet/FLUKA andSibyll/FLUKA simulations have been found.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Many organizations aspire to adopt agile processes to take advantage of thenumerous benefits that it offers to an organization. Those benefits include,but are not limited to, quicker return on investment, better software quality,and higher customer satisfaction. To date however, there is no structuredprocess (at least in the public domain) that guides organizations in adoptingagile practices. To address this problem we present the Agile AdoptionFramework. The framework consists of two components: an agile measurementindex, and a 4-Stage process, that together guide and assist the agile adoptionefforts of organizations. More specifically, the agile measurement index isused to identify the agile potential of projects and organizations. The 4-Stageprocess, on the other hand, helps determine (a) whether or not organizationsare ready for agile adoption, and (b) guided by their potential, what set ofagile practices can and should be introduced.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We consider constraints on the planetesimal population residing in the disksof AU Microscopii, Beta Pictoris and Fomalhaut taking into account theirobserved thicknesses and normal disk opacities. We estimate that bodies ofradius 5, 180 and 70 km are responsible for initiating the collisional cascadeaccounting for the dust production for AU-Mic, Beta-Pic and Fomalhaut's disks,respectively, at break radii from the star where their surface brightnessprofiles change slope. Larger bodies, of radius 1000km and with surface densityof order 0.01 g/cm^2, are required to explain the thickness of these disksassuming that they are heated by gravitational stirring. A comparison betweenthe densities of the two sizes suggests the size distribution in the largestbodies is flatter than that observed in the Kuiper belt. AU Mic's disk requiresthe shallowest size distribution for bodies with radius greater than 10kmsuggesting that the disk contains planetary embryos experiencing a stage ofrunaway growth.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "In spectroscopy, it is conventional to treat pulses much stronger than thelinewidth as delta-functions. In NMR, this assumption leads to the predictionthat pi pulses do not refocus the dipolar coupling. However, NMR spin echomeasurements in dipolar solids defy these conventional expectations when morethan one pi pulse is used. Observed effects include a long tail in the CPMGecho train for short delays between pi pulses, an even-odd asymmetry in theecho amplitudes for long delays, an unusual fingerprint pattern forintermediate delays, and a strong sensitivity to pi-pulse phase. Experimentsthat set limits on possible extrinsic causes for the phenomena are reported. Wefind that the action of the system's internal Hamiltonian during any real pulseis sufficient to cause the effects. Exact numerical calculations, combined withaverage Hamiltonian theory, identify novel terms that are sensitive toparameters such as pulse phase, dipolar coupling, and system size.Visualization of the entire density matrix shows a unique flow of quantumcoherence from non-observable to observable channels when applying repeated pipulses.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Three-body resonances in the \\bar{K}NN system have been studied within aframework of the \\bar{K}NN-\\pi YN coupled hannel Faddeev equation. By solvingthe three-body equation the energy dependence of the resonant \\bar{K}Namplitude is fully taken into account. The S-matrix pole has been investigatedfrom the eigenvalue of the kernel with the analytic continuation of thescattering amplitude on the unphysical Riemann sheet. The \\barKN interaction isconstructed from the leading order term of the chiral Lagrangian usingrelativistic kinematics. The \\Lambda(1405) resonance is dynamically generatedin this model, where the \\bar{K}N interaction parameters are fitted to the dataof scattering length. As a result we find a three-body resonance of the strangedibaryon system with binding energy, B~79 MeV, and width, \\Gamma~74 MeV. Theenergy of the three-body resonance is found to be sensitive to the model of theI=0 \\barKN interaction.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Structure entails function and thus a structural description of the brainwill help to understand its function and may provide insights into manyproperties of brain systems, from their robustness and recovery from damage, totheir dynamics and even their evolution. Advances in the analysis of complexnetworks provide useful new approaches to understanding structural andfunctional properties of brain networks. Structural properties of networksrecently described allow their characterization as small-world, random(exponential) and scale-free. They complement the set of other properties thathave been explored in the context of brain connectivity, such as topology,hodology, clustering, and hierarchical organization. Here we apply new networkanalysis methods to cortical inter-areal connectivity networks for the cat andmacaque brains. We compare these corticocortical fibre networks to benchmarkrewired, small-world, scale-free and random networks, using two analysisstrategies, in which we measure the effects of the removal of nodes andconnections on the structural properties of the cortical networks. The brainnetworks' structural decay is in most respects similar to that of scale-freenetworks. The results implicate highly connected hub-nodes and bottleneckconnections as structural basis for some of the conditional robustness of brainsystems. This informs the understanding of the development of brain networks'connectivity.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Is it possible to link a set of nodes without using preexisting positionalinformation or any kind of long-range attraction of the nodes? Can the processof generating positional information, i.e. the detection of ``unknown'' nodesand the estabishment of chemical gradients, \\emph{and} the process of networkformation, i.e. the establishment of links between nodes, occur in parallel, ona comparable time scale, as a process of co-evolution?  The paper discusses a model where the generation of relevant information forestablishing the links between nodes results from the interaction of many\\emph{agents}, i.e. subunits of the system that are capable of performing someactivities. Their collective interaction is based on (indirect) communication,which also includes memory effects and the dissemination of information in thesystem. The relevant (``pragmatic'') information that leads to theestablishment of the links then emerges from an evolutionary interplay ofselection and reamplification.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We investigate the properties and evolution of accretion tori formed afterthe coalescence of two compact objects. At these extreme densities andtemperatures, the accreting torus is cooled mainly by neutrino emissionproduced primarily by electron and positron capture on nucleons (betareactions). We solve for the disc structure and its time evolution byintroducing a detailed treatment of the equation of state which includesphotodisintegration of helium, the condition of beta-equilibrium, and neutrinoopacities. We self-consistently calculate the chemical equilibrium in the gasconsisting of helium, free protons, neutrons and electron-positron pairs andcompute the chemical potentials of the species, as well as the electronfraction throughout the disc. We find that, for sufficiently large accretionrates (> 10 solar masses per second), the inner regions of the disk becomeopaque and develop a viscous and thermal instability. The identification ofthis instability might be relevant for GRB observations.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We propose that the CP violating phase in the CKM mixing matrix is identicalto the CP phases responsible for the spontaneous CP violation in the Higgspotential. A specific multi-Higgs model with Peccei-Quinn (PQ) symmetry isconstructed to realize this idea. The CP violating phase does not vanish whenall Higgs masses become large. There are flavor changing neutral current (FCNC)interactions mediated by neutral Higgs bosons at the tree level. However,unlike general multi-Higgs models, the FCNC Yukawa couplings are fixed in termsof the quark masses and CKM mixing angles. Implications for meson-anti-mesonmixing, including recent data on $D-\\bar D$ mixing, and neutron electric dipolemoment (EDM) are studied. We find that the neutral Higgs boson masses can be atthe order of one hundred GeV. The neutron EDM can be close to the presentexperimental upper bound.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The differing M_bh-Luminosity relations presented in McLure & Dunlop, Marconi& Hunt and Erwin et al. have been investigated. A number of issues have beenidentified and addressed in each of these studies, including but not limitedto: the removal of a dependency on the Hubble constant; a correction for dustattenuation in the bulges of disc galaxies; the identification of lenticulargalaxies previously treated as elliptical galaxies; and application of the same(Y|X) regression analysis. These adjustments result in relations which nowpredict similar black hole masses. The optimal K-band relation islog(M_bh/M_sun) = -0.37(+/-0.04)[M_K +24] + 8.29(+/-0.08), with a total (notintrinsic) scatter in log M_bh equal to 0.33 dex. This level of scatter issimilar to the value of 0.34 dex from the M_bh-sigma relation of Tremaine etal. and compares favourably with the value of 0.31 dex from the M_bh-n relationof Graham & Driver. Using different photometric data, consistent relations inthe B- and R-band are also provided, although we do note that the small (N=13)R-band sample used by Erwin et al. is found here to have a slope of-0.30(+/-0.06) and a total scatter of 0.31 dex. Performing a symmetricalregression on the larger K-band sample gives a slope of -0.40, implying M_bh ~L^{1.00}. Implications for galaxy-black hole coevolution, in terms of drymergers, are briefly discussed, as are predictions for intermediate mass blackholes. Finally, as previously noted by Tundo et al., a potential bias in thegalaxy sample used to define the M_bh-L relations is shown and a correctiveformula provided.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present cosmological hydrodynamical simulations of galaxy clusters aimedat studying the process of metal enrichment of the intra--cluster medium (ICM).These simulations have been performed by implementing a detailed model ofchemical evolution in the Tree-SPH \\gd code. This model allows us to follow themetal release from SNII, SNIa and AGB stars, by properly accounting for thelifetimes of stars of different mass, as well as to change the stellar initialmass function (IMF), the lifetime function and the stellar yields. As such, ourimplementation of chemical evolution represents a powerful instrument to followthe cosmic history of metal production. The simulations presented here havebeen performed with the twofold aim of checking numerical effects, as well asthe impact of changing the model of chemical evolution and the efficiency ofstellar feedback.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present a catalogue of morphologically classified bright galaxies in thenorth equatorial stripe (230 deg$^2$) derived from the Third Data Release ofthe Sloan Digital Sky Survey (SDSS). Morphological classification is performedby visual inspection of images in the $g$ band. The catalogue contains 2253galaxies complete to a magnitude limit of $r=16$ after Galactic extinctioncorrection, selected from 2658 objects that are judged as extended in thephotometric catalogue in the same magnitude limit. 1866 galaxies in ourcatalogue have spectroscopic information. A brief statistical analysis ispresented for the frequency of morphological types and mean colours in thecatalogue. A visual inspection of the images reveals that the rate ofinteracting galaxies in the local Universe is approximately 1.5% in the$r\\le16$ sample. A verification is made for the photometric catalogue generatedby the SDSS, especially as to its bright end completeness.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The assessment of highly-risky situations at road intersections have beenrecently revealed as an important research topic within the context of theautomotive industry. In this paper we shall introduce a novel approach tocompute risk functions by using a combination of a highly non-linear processingmodel in conjunction with a powerful information encoding procedure.Specifically, the elements of information either static or dynamic that appearin a road intersection scene are encoded by using directed positional acycliclabeled graphs. The risk assessment problem is then reformulated in terms of aninductive learning task carried out by a recursive neural network. Recursiveneural networks are connectionist models capable of solving supervised andnon-supervised learning problems represented by directed ordered acyclicgraphs. The potential of this novel approach is demonstrated through wellpredefined scenarios. The major difference of our approach compared to othersis expressed by the fact of learning the structure of the risk. Furthermore,the combination of a rich information encoding procedure with a generalizedmodel of dynamical recurrent networks permit us, as we shall demonstrate, asophisticated processing of information that we believe as being a first stepfor building future advanced intersection safety systems", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We study the mechanical response generated by local deformations in jammedpackings of rigid disks. Based on discrete element simulations we determine thecritical force of the local perturbation that is needed to break the mechanicalequilibrium and examine the generated displacement field. Displacements decayas a power law of the distance from the perturbation point. The decay exponentand the critical force exhibit nontrivial dependence on the friction: Bothquantities are nonmonotonic and have a sharp maximum at the frictioncoefficient 0.1. We find that the mechanical response properties are closelyrelated to the problem of force-indeterminacy where similar nonmonotonicbehavior was observed previously. We establish direct connection between thecritical force and the ensemble of static force networks.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "During the epoch of reionization, the formation of radiation sources isaccompanied by the growth of a H- photodissociating flux. We estimate theimpact of this flux on the formation of molecular hydrogen and cooling in thefirst galaxies, assuming different types of radiation sources (e.g. Pop II andPop III stars, miniquasars). We find that H- photodissociation reduces theformation of H2 molecules by a factor of ~1+1000k_s*x/(f_esc*delta), where x isthe mean ionized fraction in the IGM, f_esc is the fraction of ionizing photonsthat escape from their progenitor halos, delta is the local gas overdensity andk_s is an order unity constant which depends on the type of radiation source.By the time a significant fraction of the universe becomes ionized, H-photodissociation may significantly reduce the H2 abundance and, with it, theprimordial star formation rate, delaying the progress of reionization.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present new predictions for the galaxy three-point correlation function(3PCF) using high-resolution dissipationless cosmological simulations of a flatLCDM Universe which resolve galaxy-size halos and subhalos. We create realisticmock galaxy catalogs by assigning luminosities and colors to dark matter halosand subhalos, and we measure the reduced 3PCF as a function of luminosity andcolor in both real and redshift space. As galaxy luminosity and color arevaried, we find small differences in the amplitude and shape dependence of thereduced 3PCF, at a level qualitatively consistent with recent measurements fromthe SDSS and 2dFGRS. We confirm that discrepancies between previous 3PCFmeasurements can be explained in part by differences in binning choices. Weexplore the degree to which a simple local bias model can fit the simulated3PCF. The agreement between the model predictions and galaxy 3PCF measurementslends further credence to the straightforward association of galaxies with CDMhalos and subhalos.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "This paper aims to provide a practical example on the assessment andpropagation of input uncertainty for option pricing when using tree-basedmethods. Input uncertainty is propagated into output uncertainty, reflectingthat option prices are as unknown as the inputs they are based on. Optionpricing formulas are tools whose validity is conditional not only on how closethe model represents reality, but also on the quality of the inputs they use,and those inputs are usually not observable. We provide three alternativeframeworks to calibrate option pricing tree models, propagating parameteruncertainty into the resulting option prices. We finally compare our methodswith classical calibration-based results assuming that there is no optionsmarket established. These methods can be applied to pricing of instruments forwhich there is not an options market, as well as a methodological tool toaccount for parameter and model uncertainty in theoretical option pricing.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Context: HCOOH is one of the more common species in interstellar ices withabundances of 1-5% with respect to solid H2O. Aims: This study aims atcharacterizing the HCOOH spectral features in astrophysically relevant icemixtures in order to interpret astronomical data. Methods: The ices are grownunder high vacuum conditions and spectra are recorded in transmission using aFourier transform infrared spectrometer. Pure HCOOH ices deposited at 15 K and145 K are studied, as well as binary and tertiary mixtures containing H2O, CO,CO2 and CH3OH. The mixture concentrations are varied from 50:50% to ~10:90% forHCOOH:H2O. Binary mixtures of HCOOH:X and tertiary mixtures of HCOOH:H2O:X withX = CO, CO2, and CH3OH, are studied for concentrations of ~10:90% and~7:67:26%, respectively. Results: Pure HCOOH ice spectra show broad bands whichsplit around 120 K due to the conversion of a dimer to a chain-structure. Broadsingle component bands are found for mixtures with H2O. Additional spectralcomponents are present in mixtures with CO, CO2 and CH3OH. The resulting peakposition, full width at half maximum and band strength depend strongly on icestructure, temperature, matrix constituents and the HCOOH concentration.Comparison of the solid HCOOH 5.9, 7.2, and 8.1 micron features withastronomical data toward the low mass source HH 46 and high mass source W 33Ashows that spectra of binary mixtures do not reproduce the observed icefeatures. However, our tertiary mixtures especially with CH3OH match theastronomical data very well. Thus interstellar HCOOH is most likely present intertiary or more complex mixtures with H2O, CH3OH and potentially also CO orCO2, providing constraints on its formation.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Presently clearing electrodes are being considered as a possible cure ofe-cloud driven problems in existing and future colliders. 'Invisible'electrodes, made of a thin highly resistive layer pasted on a dielectric plate,have been proposed as one of design solutions for the e-cloud clearing. For thefirst time such electrodes were successfully used in the electron-positronaccumulator (EPA) of LEP. Similar electrodes had been using for a long time forion clearing purposes in the DAFNE electron ring. Theoretical considerationsand experimental measurements at DAFNE have revealed a substantial contributionof the ion clearing electrodes (ICE) to the machine broad-band impedance givingrise to several harmful effects degrading the collider performance. In thispaper we discuss the impact of the electrodes on DAFNE beam dynamics, show theresults of ICE wake field and impedance calculations and compare them withavailable experimental data. We also describe the procedure of ICE removal fromthe wiggler sections of the electron ring that has resulted in remarkableimprovements in terms of beam dynamics and geometric luminosity.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Scaling predictions and results from self-consistent field calculations forbottle-brush polymers with a rigid backbone and flexible side chains under goodsolvent conditions are summarized and their validity and applicability isassessed by a comparison with Monte Carlo simulations of a simple latticemodel. It is shown that under typical conditions, as they are also present inexperiments, only a rather weak stretching of the side chains is realized, andthen the scaling predictions based on the extension of the Daoud-Cotton blobpicture are not applicable.  Also two-component bottle brush polymers are considered, where two types(A,B) of side chains are grafted, assuming that monomers of different kindrepel each other. In this case, variable solvent quality is allowed for, suchthat for poor solvent conditions rather dense cylinder-like structures result.Theories predict ``Janus Cylinder''-type phase separation along the backbone inthis case. The Monte Carlo simulations, using the pruned-enriched Rosenbluthmethod (PERM) then are restricted to rather short side chain length.Nevertheless, evidence is obtained that the phase separation between an A-richpart of the cylindrical molecule and a B-rich part can only occur locally. Thecorrelation length of this microphase separation can be controlled by thesolvent quality. This lack of a phase transition is interpreted by an analogywith models for ferromagnets in one space dimension.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We prove the Kirillov-Reshetikhin (KR) conjecture in the general case : forall twisted quantum affine algebras we prove that the characters of KR modulessolve the twisted Q-system and we get explicit formulas for the character oftheir tensor products (the untwisted simply-laced case was treated by Najakima,and the untwisted case by the author). The proof is uniform and providesseveral new developments for the representation theory of twisted quantumaffine algebras, including twisted Frenkel-Reshetikhin q-characters (expectedby Frenkel-Reshetikhin and Frenkel-Mukhin). We also prove the twisted T-system.As an application we get explicit formulas for the twisted q-characters offundamental representations for all types, including the formulas for typesD_4^{(3)}, E_6^{(2)} conjectured by Reshetikhin. We prove the formulas for KRmodules in types A_n^{(2)} and D_4^{(3)} conjectured by Kuniba-Suzuki.Eventually our results imply the conjectural branching rules [HKOTT] to thequantum subalgebra of finite type.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The gargantuan discrepancy between the value of the observed cosmologicalconstant and that expected from the zero-point energy of known matter fieldscan be eliminated by supposing that on macroscopic scales the overwhelmingmajority of any volume of spacetime is literal nothingness. This nothingness orvoid results from the proliferative nucleation of tiny void bubbles (a.k.a.\"bubbles of nothing\" or \"semi wormholes\") that expand until their surfaces,presumed to be 2-branes, collide. This process results in a dense packing ofvoid bubbles of various sizes that leaves only the vanishing interstitialregions between bubbles for spacetime to occupy. This vast reduction in theamount of actual space contained within any apparent volume, reducescorrespondingly the effective zero-point energy density. Unlike previouswormhole-based attempts at vacuum energy suppression, the current approach isentirely Lorentzian and results in a nonzero value for the cosmologicalconstant.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present a study of eegamma and mumugamma events using 1109 (1009) pb-1 ofdata in the electron (muon) channel, respectively. These data were collectedwith the D0 detector at the Fermilab Tevatron ppbar Collider at sqrt(s) = 1.96TeV. Having observed 453 (515) candidates in the eegamma (mumugamma) finalstate, we measure the Zgamma production cross section for a photon withtransverse energy ET > 7 GeV, separation between the photon and leptons DeltaR(lgamma) > 0.7, and invariant mass of the di-lepton pair M(ll) > 30 GeV/c^2,to be 4.96 +/- 0.30(stat. + syst.) +/- 0.30(lumi.) pb, in agreement with thestandard model prediction of 4.74 +/- 0.22 pb. This is the most precise Zgammacross section measurement at a hadron collider. We set limits on anomaloustrilinear Zgammagamma and ZZgamma gauge boson couplings of -0.085 <h(30)^(gamma) < 0.084, -0.0053 < h(40)^(gamma) < 0.0054 and -0.083 < h(30)^(Z)< 0.082, -0.0053 < h(40)^(Z) < 0.0054 at the 95% C.L. for the form-factor scaleLambda = 1.2 TeV.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present the first systematic investigation of the [NeV] (14um/24um) and[SIII] (18um/33um) infrared line flux ratios, traditionally used to estimatethe density of the ionized gas, in a sample of 41 Type 1 and Type 2 activegalactic nuclei (AGNs) observed with the Infrared Spectrograph on boardSpitzer. The majority of galaxies with both [NeV] lines detected have observed[NeV] line flux ratios consistent with or below the theoretical low densitylimit, based on calculations using currently available collision strengths andignoring absorption and stimulated emission. We find that Type 2 AGNs havelower line flux ratios than Type 1 AGNs and that all of the galaxies with lineflux ratios below the low density limit are Type 2 AGNs. We argue thatdifferential infrared extinction to the [NeV] emitting region due to dust inthe obscuring torus is responsible for the ratios below the low density limitand we suggest that the ratio may be a tracer of the inclination angle of thetorus to our line of sight. Because the temperature of the gas, the amount ofextinction, and the effect of absorption and stimulated emission on the lineratios are all unknown, we are not able to determine the electron densitiesassociated with the [NeV] line flux ratios for the objects in our sample. Wealso find that the [SIII] emission from the galaxies in our sample is extendedand originates primarily in star forming regions. Since the emission fromlow-ionization species is extended, any analysis using line flux ratios fromsuch species obtained from slits of different sizes is invalid for most nearbygalaxies.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The Large Area Telescope (LAT) instrument onboard GLAST offers a tremendousopportunity for future blazar studies. In order to fully benefit from itscapabilities and to maximize the scientific return from the LAT, it is of greatimportance to conduct dedicated multi-frequency monitoring campaigns that willresult comprehensive observations. Consequently, we initiated an effort toconduct a GLAST-dedicated, quasi-simultaneous, broad-band flux-density (andpolarization) monitoring of potential GLAST blazars with the Effelsberg andOVRO radio telescopes (11cm to 7mm wavelength). Here, we present a shortoverview of these activities which will complement the multi-wavelengthsactivities of the GLAST/LAT collaboration towards the 'low-energy' radio bands.Further we will give a brief outlook including the extension of thiscoordinated campaign towards higher frequencies and future scientific aims.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Position determination in biological systems is often achieved throughprotein concentration gradients. Measuring the local concentration of such aprotein with a spatially-varying distribution allows the measurement ofposition within the system. In order for these systems to work effectively,position determination must be robust to noise. Here, we calculate fundamentallimits to the precision of position determination by concentration gradientsdue to unavoidable biochemical noise perturbing the gradients. We focus ongradient proteins with first order reaction kinetics. Systems of this type havebeen experimentally characterised in both developmental and cell biologysettings. For a single gradient we show that, through time-averaging, greatprecision can potentially be achieved even with very low protein copy numbers.As a second example, we investigate the ability of a system with oppositelydirected gradients to find its centre. With this mechanism, positionalprecision close to the centre improves more slowly with increasing averagingtime, and so longer averaging times or higher copy numbers are required forhigh precision. For both single and double gradients, we demonstrate theexistence of optimal length scales for the gradients, where precision ismaximized, as well as analyzing how precision depends on the size of theconcentration measuring apparatus. Our results provide fundamental constraintson the positional precision supplied by concentration gradients in variouscontexts, including both in developmental biology and also within a singlecell.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Very much like the ubiquitous quantum interference of a single particle withitself, quantum interference of two independent, but indistinguishable,particles is also possible. This interference is a direct result of quantumexchange statistics, however, it is observed only in the joint probability tofind the particles in two separated detectors. Here we report the firstobservation of such interference fringes between two independent andnon-interacting electrons in an interferometer proposed by Yurke et al. andSamuelsson et al. Our experiment resembles the \"Hanbury Brown and Twiss\" (HBT)experiment, which was performed with classical waves. In the experiment, twoindependent and mutually incoherent electron beams were each partitioned intotwo trajectories. The combined four trajectories enclosed an Aharonov-Bohm (AB)flux (but not the two trajectories of a single electron). While individualcurrents were found to be independent of the AB flux, as expected, thecross-correlation between current fluctuations in two opposite points acrossthe device exhibited strong AB oscillations. This is a direct signature oforbital entanglement between two electrons even though they never interact witheach other.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The extraordinary astrometric accuracy of radio interferometry creates animportant and unique opportunity for the discovery and characterization ofexo-planets. Currently, the Very Long Baseline Array can routinely achievebetter than 100 microarcsecond accuracy, and can approach 10 microarcsecondwith careful calibration. We describe here RIPL, the Radio InterferometricPLanet search, a new program with the VLBA and the Green Bank 100 m telescopethat will survey 29 low-mass, active stars over 3 years with sub-Jovian planetmass sensitivity at 1 AU. An upgrade of the VLBA bandwidth will increaseastrometric accuracy by an order of magnitude. Ultimately, the colossalcollecting area of the Square Kilometer Array could push astrometric accuracyto 1 microarcsecond, making detection and characterizaiton of Earth massplanets possible.  RIPL and other future radio astrometric planet searches occupy a uniquevolume in planet discovery and characterization parameter space. The parameterspace of astrometric searches gives greater sensitivity to planets at largeradii than radial velocity searches. For the VLBA and the expanded VLBA, thetargets of radio astrometric surveys are by necessity nearby, low-mass, activestars, which cannot be studied efficiently through the radial velocity method,coronagraphy, or optical interferometry. For the SKA, detection sensitivitywill extend to solar-type stars. Planets discovered through radio astrometricmethods will be suitable for characterization through extreme adaptive optics.  The complementarity of radio astrometric techniques with other methodsdemonstrates that radio astrometry can play an important role in the roadmapfor exoplanet discovery and characterization.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We propose a method to study the epoch of reionization based on the possibleobservation of 2p--2s fine structure lines from the neutral hydrogen outsidethe cosmological H {\\sc ii} regions enveloping QSOs and other ionizing sourcesin the reionization era. We show that for parameters typical of luminoussources observed at $z \\simeq 6.3$ the strength of this signal, which isproportional to the H {\\sc i} fraction, has a brightness temperature $\\simeq 20  \\mu K$ for a fully neutral medium. The fine structure line from this redshiftis observable at $\\nu \\simeq 1 \\rm GHz$ and we discuss prospects for thedetection with several operational and future radio telescopes. We also computethe characteristics of this signal from the epoch of recombination: the peakbrightness is expected to be $\\simeq 100 \\mu K$; this signal appears in thefrequency range 5-10 MHz. The signal from the recombination era is nearlyimpossible to detect owing to the extreme brightness of the Galactic emissionat these frequencies.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Following the recent insight in the material structure of comets,protoplanetesimals are assumed to have low densities and to be highly porousagglomerates. It is still unclear if planetesimals can be formed from theseobjects by collisional growth. Therefore, it is important to study numericallythe collisional outcome from low velocity impacts of equal sized porousagglomerates which are too large to be examined in a laboratory experiment. Weuse the Lagrangian particle method Smooth Particle Hydrodynamics to solve theequations that describe the dynamics of elastic and plastic bodies.Additionally, to account for the influence of porosity, we follow a previousdeveloped equation of state and certain relations between the material strengthand the relative density. Collisional growth seems possible for rather lowcollision velocities and particular material strengths. The remnants ofcollisions with impact parameters that are larger than 50% of the radius of thecolliding objects tend to rotate. For small impact parameters, the collidingobjects are effectively slowed down without a prominent compaction of theporous structure, which probably increases the possibility for growth. Theprotoplanetesimals, however, do not stick together for the most part of theemployed material strengths. An important issue in subsequent studies has to bethe influence of rotation to collisional growth. Moreover, for realisticsimulations of protoplanetesimals it is crucial to know the correct materialparameters in more detail.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Author details research on the new, very prospective, electrostatic SpaceElevator climber based on a new electrostatic linear engine previously offeredat the 42nd Joint Propulsion Conference (AIAA-2006-5229) and published in AEAT,Vol.78, No.6, 2006, pp. 502-508. The electrostatic climber discussed can haveany speed (and braking), the energy for climber movement is delivered by alightweight high-voltage line into a Space Elevator-holding cable from Earthelectric generator. This electric line also can be used for delivery electricenergy to a Geosynchronous Space Station. At present, the best solution of theclimber problem (announced by NASA as one important awarding problem of SpaceElevator) is problematic.  Author also shows the linear electrostatic engine may be used as realisticpower space launcher at the present time. Two projects illustrate these newdevices.  Key words: Space elevator, Electrostatic climber for space elevator,Electrostatic space launcher, Electrostatic accelerator.  This work is presented as paper AIAA-2007-5838 for 43 Joint PropulsionConference, Cincinnati, Ohio, USA, 9-11 July, 2007,", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We search for galaxy counterparts to damped Lyman-alpha absorbers (DLAs) atz>2 towards nine quasars, which have 14 DLAs and 8 sub-DLAs in their spectra.We use integral field spectroscopy to search for Ly-alpha emission line objectsat the redshifts of the absorption systems. Besides recovering two previouslyconfirmed objects, we find six statistically significant candidate Ly-alphaemission line objects. The candidates are identified as having wavelengthsclose to the DLA line where the background quasar emission is absorbed. Incomparison with the six currently known Ly-alpha emitting DLA galaxies thecandidates have similar line fluxes and line widths, while velocity offsetsbetween the emission lines and systemic DLA redshifts are larger. The impactparameters are larger than 10 kpc, and lower column density systems are foundat larger impact parameters. Assuming that a single gas cloud extends from theQSO line of sight to the location of the candidate emission line, we find thatthe average candidate DLA galaxy is surrounded by neutral gas with anexponential scale length of ~5 kpc.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "This paper compares two neural network input selection schemes, the PrincipalComponent Analysis (PCA) and the Automatic Relevance Determination (ARD) basedon Mac-Kay's evidence framework. The PCA takes all the input data and projectsit onto a lower dimension space, thereby reduc-ing the dimension of the inputspace. This input reduction method often results with parameters that havesignificant influence on the dynamics of the data being diluted by those thatdo not influence the dynamics of the data. The ARD selects the most relevantinput parameters and discards those that do not contribute significantly to thedynamics of the data being modelled. The ARD sometimes results with importantinput parameters being discarded thereby compromising the dynamics of the data.The PCA and ARD methods are implemented together with a Multi-Layer-Perceptron(MLP) network for fault identification in structures and the performance of thetwo methods is as-sessed. It is observed that ARD and PCA give similaraccu-racy levels when used as input-selection schemes. There-fore, the choiceof input-selection scheme is dependent on the nature of the data beingprocessed.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Electronic structure of stripe ordered La$_{2-x}$Sr$_{x}$NiO$_{4}$ isinvestigated. The system with x=1/3 is insulator, in LSDA+U calculations, andshows charge and spin stripe, consistent with the experimental results. Highlycorrelated system of x=1/2 is studied by using exact diagonalization ofmulti-orbital many body Hamiltonian derived from LDA calculations and includingon-site and inter-site Coulomb interactions. The fluctuation of the residualspin on Ni$^{3+}$ (hole) site couples with the charge fluctuation betweenNi$^{3+}$ and Ni$^{2+}$ states and this correlation lowers the total energy.The resultant ground state is insulator with charge and spin stripe of theenergy gap 0.9eV, consistent with observed one. The on-site Coulomb interactionstabilizes integral valency of each Ni ion (Ni$^{3+}$ and Ni$^{2+}$), but doesnot induce the charge order. Two quantities, inter-site Coulomb interaction andanisotropy of hopping integrals, play an important role to form the charge andspin stripe order in a system of x=1/2.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We determine the masses and decay constants of the pseudoscalar mesons Bs andBc, and also the masses of the vector mesons Bs^* and Bc^*, in quenched latticeQCD with exact chiral symmetry. For 100 gauge configurations generated withsingle-plaquette action at beta = 7.2 on the 32^3 x 60 lattice, we computepoint-to-point quark propagators for 33 quark masses in the range [0.01, 0.85],and measure the time-correlation functions of pseudoscalar and vector mesons.The inverse lattice spacing and the charm quark bare mass are determined usingthe mass and decay constant of eta_c(2980). The bare masses of s and b quarksare chosen such that the masses of the corresponding vector mesons are in goodagreement with phi(1020), and Upsilon(9460) respectively. Our results are:m_{Bs} = 5385(27)(17) MeV, f_{Bs} = 253(8)(7) MeV, m_{Bc} = 6278(6)(4) MeV,f_{Bc} = 489(4)(3) MeV, m_{Bs^*} = 5424(28)(19) MeV, and m_{Bc^*} = 6315(6)(5)MeV.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We discuss the impact of charged massive particle big bangnucleosynthesis(CBBN) to explore the nature of the reheating of the Universe inthe case that a new extremely long-lived charged massive particle(CHAMP)exists. If the mass of the CHAMP is within collider reach and it's lifetime islonger than $10^4$sec, the comparison between the CBBN prediction and observed$^6$Li abundances may indicate nonstandard reheating in the early Universewithout relying on details of the decay properties. Even if the CHAMP mass isoutside the reach of colliders, the cosmological considerations may provide anontrivial hint for the existence of such very heavy long-lived CHAMPs from thelate Universe if the daughter particles are the dominant component of thepresent dark matter. We consider a low reheating temperature model as anexample of the nonstandard reheating scenarios.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We consider a stationary and ergodic random field {\\omega(b)} parameterizedby the family of bonds b in Z^d, d>1. The random variable \\omega(b) is thoughtof as the conductance of bond b and it ranges in a finite interval [0,c_0].Assuming that the set of bonds with positive conductance has a unique infinitecluster C, we prove homogenization results for the random walk among randomconductances on C. As a byproduct, applying the general criterion of \\cite{F}leading to the hydrodynamic limit of exclusion processes with bond-dependenttransition rates, for almost all realizations of the environment we prove thehydrodynamic limit of simple exclusion processes among random conductances onC. The hydrodynamic equation is given by a heat equation whose diffusion matrixdoes not depend on the environment. We do not require any ellipticitycondition. As special case, C can be the infinite cluster of supercriticalBernoulli bond percolation.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Using a semi-analytical model for galaxy formation, combined with a largeN-body simulation, we investigate the origin of the dichotomy among early-typegalaxies. We find that boxy galaxies originate from mergers with a progenitormass ratio $n < 2$ and with a combined cold gas mass fraction $F_{\\rm cold} <0.1$. Our model accurately reproduces the observed fraction of boxy systems asa function of luminosity and halo mass, for both central galaxies andsatellites. After correcting for the stellar mass dependence, the properties ofthe last major merger of early-type galaxies are independent of their halomass. This provides theoretical support for the conjecture of Pasquali et al(2007) that the stellar mass of an early-type galaxy is the main parameter thatgoverns its isophotal shape. We argue that the observed dichotomy of early-typegalaxies has a natural explanation within hierarchical structure formation, anddoes not require AGN feedback. Rather, we argue that it owes to the fact thatmore massive systems (i) have more massive progenitors, (ii) assemble later,and (iii) have a larger fraction of early-type progenitors. Each of these threetrends causes the cold gas mass fraction of the progenitors of more massiveearly-types to be lower, so that their last major merger was dryer. Finally,our model predicts that (i) less than 10 percent of all early-type galaxiesform in major mergers that involve two early-type progenitors, (ii) more than95 percent of all boxy early-type galaxies with $M_* < 2 \\times 10^{10} h^{-1}\\Msun$ are satellite galaxies, and (iii) about 70 percent of all low massearly-types do not form a supermassive black hole binary at their last majormerger. The latter may help to explain why low mass early-types have centralcusps, while their massive counterparts have cores.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Color confinement and chiral symmetry specify some important territory forthe study of hadronic physics. Any hadron can be defined as a color-singletcomposite system of qurks and gluons, the fundamental fields of qcd, while thelandscape of the hadronic spectrum is dominated by the fact that two quarkflavors, u and d, are characterized by masses small compared to the fundamentalscale of this theory. Measurements sensitive to the orbital angular momenta ofthe color constituents of the nucleon display the interplay of chiral dynamicsand confinement in a unique manner. This pageant can be explored by anevaluation, within the context of the Georgi-Manohar chiral quark model, of thenormalization of the orbital structure functions and the normalization of theBoer-Mulders functions for different quark flavors. The resolution structuresin the chiral quark model represent an evaluation of Collins functions for aconfined system defined by the quantum numbers of the nucleon in theconstituent quark model. The orbital structure functions for antiquarks canalso be specified within the basic framework of this approach while thenormalization of the gluon orbital structure function requires some additionalassumptions.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present observations and modeling of a lunar occultation of thedust-enshrouded carbon star AFGL 5440. The observations were made over acontinuous range of wavelengths from 1 - 4um with a high-speedspectrophotometer designed expressly for this purpose. We find that theoccultation fringes cannot be fit by any single-size model. We use the DUSTYradiative transfer code to model a circumstellar shell and fit both theobserved occultation light curves and the spectral energy distributiondescribed in the literature. We find a strong constraint on the inner radius ofthe dust shell, Tmax = 950 K +/- 50K, and optical depth at 5um of 0.5 +/- 0.1.The observations are best fit by models with a density gradient of r^-2 or thegradient derived by Ivezic & Elitzur for a radiatively driven hydrodynamicoutflow. Our models cannot fit the observed IRAS 60um flux without assuming asubstantial abundance of graphite or by assuming a substantially highermass-loss rate in the past.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The blasting of brittle materials with sharp particles is an importantfabrication technology in many industrial processes. In particular, formicro-systems, it allows the production of devices with feature sizes down tofew tens of microns. An important parameter of this process is the surfaceroughness of post-blasted surfaces. In this work the scaling properties ofPyrex glass and silicon surfaces after bombardment with alumina particles isinvestigated. The targets were bombarded at normal incidence using aluminaparticles with two different average sizes, $29\\mu m$ and $9\\mu m$,respectively. This investigation indicates that the resulting surfaces havemultifractal properties. Applying multifractal detrended fluctuation analysis(MFDFA) allowed us to determine the singularity spectrum of the surfaces. Thisspectrum did not depend on the target material or on the size of the particles.Several parameters quantifying relevant quantities were determined. We arguethat for scales below $5 \\mu m$, fracture processes are dominant while at largescales long range correlations are responsible for the multifractal behaviour.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Context: The mass-loss rate is a key parameter of massive stars. Adequatestellar atmosphere models are required for spectral analyses and mass-lossdeterminations. Present models can only account for the inhomogeneity ofstellar winds in the approximation of small-scale structures that are opticallythin. This treatment of ``microclumping'' has led to reducing empiricalmass-loss rates by factors of two and more. Aims: Stellar wind clumps can beoptically thick in spectral lines. We investigate how this ``macroclumping''impacts on empirical mass-loss rates. Methods: The Potsdam Wolf-Rayet (PoWR)model atmosphere code is generalized in the ``formal integral'' to account forclumps that are not necessarily optically thin. Results: Optically thick clumpsreduce the effective opacity. This has a pronounced effect on the emergentspectrum. Our modeling for the O-type supergiant zeta Puppis reveals that theoptically thin H-alpha line is not affected by wind porosity, but that the PVresonance doublet becomes significantly weaker when macroclumping is taken intoaccount. The reported discrepancies between resonance-line andrecombination-line diagnostics can be resolved entirely with the macroclumpingmodeling without downward revision of the mass-loss rate. Conclusions:Mass-loss rates inferred from optically thin emission, such as the H-alpha linein O stars, are not influenced by macroclumping. The strength of opticallythick lines, however, is reduced because of the porosity effects. Therefore,neglecting the porosity in stellar wind modeling can lead to underestimatingempirical mass-loss rates.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Let $C_a$ be the central Cantor set obtained by removing a central intervalof length $1-2a$ from the unit interval, and continuing this processinductively on each of the remaining two intervals. We prove that if $\\logb/\\log a$ is irrational, then \\[ \\dim(C_a+C_b) = \\min(\\dim(C_a) + \\dim(C_b),1),\\] where $\\dim$ is Hausdorff dimension. More generally, given two self-similarsets $K,K'$ in $\\RR$ and a scaling parameter $s>0$, if the dimension of thearithmetic sum $K+sK'$ is strictly smaller than $\\dim(K)+\\dim(K') \\le 1$(``geometric resonance''), then there exists $r<1$ such that all contractionratios of the similitudes defining $K$ and $K'$ are powers of $r$ (``algebraicresonance''). Our method also yields a new result on the projections of planarself-similar sets generated by an iterated function system that includes ascaled irrational rotation.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We explore the cosmological content of Salam-Sezgin six dimensionalsupergravity, and find a solution to the field equations in qualitativeagreement with observation of distant supernovae, primordial nucleosynthesisabundances, and recent measurements of the cosmic microwave background. Thecarrier of the acceleration in the present de Sitter epoch is a quintessencefield slowly rolling down its exponential potential. Intrinsic to this model isa second modulus which is automatically stabilized and acts as a source of colddark matter with a mass proportional to an exponential function of thequintessence field (hence realizing VAMP models within a String context).However, any attempt to saturate the present cold dark matter component in thismanner leads to unacceptable deviations from cosmological data -- a numericalstudy reveals that this source can account for up to about 7% of the total colddark matter budget. We also show that (1) the model will support a de Sitterenergy in agreement with observation at the expense of a miniscule breaking ofsupersymmetry in the compact space; (2) variations in the fine structureconstant are controlled by the stabilized modulus and are negligible; (3)``fifth''forces are carried by the stabilized modulus and are short range; (4)the long time behavior of the model in four dimensions is that of aRobertson-Walker universe with a constant expansion rate (w = -1/3). Finally,we present a String theory background by lifting our six dimensionalcosmological solution to ten dimensions.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "All maximal supergravities in four space-time dimensions are presented. Theungauged Lagrangians can be encoded in an E_7(7)\\Sp(56,R)/GL(28) matrixassociated with the freedom of performing electric/magnetic dualitytransformations. The gauging is defined in terms of an embedding tensor whichencodes the subgroup of E_7(7) that is realized as a local invariance. Thisembedding tensor may imply the presence of magnetic charges which requirecorresponding dual gauge fields. The latter can be incorporated by using arecently proposed formulation that involves tensor gauge fields in the adjointrepresentation of E_7(7). In this formulation the results take a universal formirrespective of the electric/magnetic duality basis. We present the generalclass of supersymmetric and gauge invariant Lagrangians and discuss a number ofapplications.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "By their star content, the galaxies split out into a red and a bluepopulation; their color index peaked around u-r=2.5 or u-r=1, respectively,quantifies the ratio of the blue stars newly formed from cold galactic gas, tothe redder ones left over by past generations. On the other hand, uponaccreting substantial gas amounts the central massive black holes energizeactive galactic nuclei (AGNs); here we investigate whether these show asimilar, and possibly related, bimodal partition as for current accretionactivity relative to the past. To this aim we use an updated semianalyticmodel; based on Monte Carlo simulations, this follows with a large statisticsthe galaxy assemblage, the star generations and the black hole accretions inthe cosmological framework over the redshift span from z=10 to z=0. We test oursimulations for yielding in close detail the observed split of galaxies into ared, early and a blue, late population. We find that the black hole accretionactivities likewise give rise to two source populations: early, bright quasarsand later, dimmer AGNs. We predict for their Eddington parameter $\\lambda_E$ --the ratio of the current to the past black hole accretions -- a bimodaldistribution; the two branches sit now under $\\lambda_E \\approx 0.01$ (mainlycontributed by low-luminosity AGNs) and around $\\lambda_E \\approx 0.3-1$. Thesenot only mark out the two populations of AGNs, but also will turn out tocorrelate strongly with the red or blue color of their host galaxies.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The influence of excited-state absorption (ESA) and two-exciton processes ona coherent population transfer with intense ultrashort chirped pulses inmolecular systems in solution has been studied. An unified treatment ofadiabatic rapid passage (ARP) in such systems has been developed using athree-state electronic system with relaxation treated as a diffusion onelectronic potential energy surfaces. We have shown that ESA has a profoundeffect on coherent population transfer in large molecules that necessitates amore accurate interpretation of experimental data. A simple and physicallyclear model for ARP in molecules with three electronic states in solution hasbeen developed by extending the Landau-Zener calculations putting in a thirdlevel to random crossing of levels. A method for quantum control of two-excitonstates in molecular complexes has been proposed.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "A combination of experimental techniques and molecular dynamics (MD) computersimulation is used to investigate the diffusion dynamics in Al80Ni20 melts.Experimentally, the self-diffusion coefficient of Ni is measured by thelong-capillary (LC) method and by quasielastic neutron scattering. The LCmethod yields also the interdiffusion coefficient. Whereas the experiments weredone in the normal liquid state, the simulations provided the determination ofboth self-diffusion and interdiffusion constants in the undercooled regime aswell. The simulation results show good agreement with the experimental data. Inthe temperature range 3000 K >= T >= 715 K, the interdiffusion coefficient islarger than the self-diffusion constants. Furthermore the simulation shows thatthis difference becomes larger in the undercooled regime. This result can berefered to a relatively strong temperature dependence of the thermodynamicfactor \\Phi, which describes the thermodynamic driving force forinterdiffusion. The simulations also indicate that the Darken equation is agood approximation, even in the undercooled regime. This implies that dynamiccross correlations play a minor role for the temperature range underconsideration.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "A characteristic feature of thermalized non-equilibrated matter is that, inspite of energy relaxation--equilibration, a phase memory of the way themany-body system was excited remains. As an example, we analyze data on astrong forward peaking of thermal proton yield in the Bi($\\gamma$,p)photonuclear reaction. New analysis shows that the phase relaxation inhighly-excited heavy nuclei can be 8 orders of magnitude or even much longerthan the energy relaxation. We argue that thermalized non-equilibrated matterresembles a high temperature superconducting state in quantum many-bodysystems. We briefly present results on the time-dependent correlation functionof the many-particle density fluctuations for such a superconducting state. Itshould be of interest to experimentally search for manifestations ofthermalized non-equilibrated matter in many-body mesoscopic systems andnanostructures.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The Boltzmann equation for d-dimensional inelastic Maxwell models isconsidered to analyze transport properties in spatially inhomogeneous statesclose to the simple shear flow. A normal solution is obtained via aChapman--Enskog--like expansion around a local shear flow distribution f^{(0)}that retains all the hydrodynamic orders in the shear rate. The constitutiveequations for the heat and momentum fluxes are obtained to first order in thedeviations of the hydrodynamic field gradients from their values in thereference state and the corresponding generalized transport coefficients are{\\em exactly} determined in terms of the coefficient of restitution \\alpha andthe shear rate a. Since f^{(0)} applies for arbitrary values of the shear rateand is not restricted to weak dissipation, the transport coefficients turn outto be nonlinear functions of both parameters a and \\alpha. A comparison withprevious results obtained for inelastic hard spheres from a kinetic model ofthe Boltzmann equation is also carried out.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "A recently introduced nonlinear Fokker-Planck equation, derived directly froma master equation, comes out as a very general tool to describephenomenologically systems presenting complex behavior, like anomalousdiffusion, in the presence of external forces. Such an equation ischaracterized by a nonlinear diffusion term that may present, in general, twodistinct powers of the probability distribution. Herein, we calculate thestationary-state distributions of this equation in some special cases, andintroduce associated classes of generalized entropies in order to satisfy theH-theorem. Within this approach, the parameters associated with the transitionrates of the original master-equation are related to such generalizedentropies, and are shown to obey some restrictions. Some particular cases arediscussed.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We have imaged a $\\sim$6 arcminute$^2$ region in the Bo\\\"otes Deep Fieldusing the 350 $\\mu$m-optimised second generation Submillimeter High AngularResolution Camera (SHARC II), achieving a peak 1$\\sigma$ sensitivity of $\\sim$5mJy. We detect three sources above 3$\\sigma$, and determine a spurious sourcedetection rate of 1.09 in our maps. In the absence of $5\\sigma$ detections, werely on deep 24 $\\mu$m and 20 cm imaging to deduce which sources are mostlikely to be genuine, giving two real sources. From this we derive an integralsource count of 0.84$^{+1.39}_{-0.61}$ sources arcmin$^{-2}$ at $S>13$ mJy,which is consistent with 350 $\\mu$m source count models that have anIR-luminous galaxy population evolving with redshift. We use these constraintsto consider the future for ground-based short-submillimetre surveys.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The effect of introducing a fifth large-scale space-time dimension to theequations of orbital dynamics was analysed in an earlier paper by the authors.The results showed good agreement with the observed flat rotation curves ofgalaxies and the Pioneer Anomaly. This analysis did not require themodification of Newtonian dynamics, but rather only their restatement in a fivedimensional framework. The same analysis derived a acceleration parameter ar,which plays an important role in the restated equations of orbital dynamics,and suggested a value for ar. In this companion paper, the principle ofconservation of energy is restated within the same five-dimensional framework.The resulting analysis provides an alternative route to estimating the value ofar, without reference to the equations of orbital dynamics, and based solely onkey cosmological constants and parameters, including the gravitationalconstant, G. The same analysis suggests that: (i) the inverse square law ofgravity may itself be due to the conservation of energy at the boundary betweena four-dimensional universe and a fifth large-scale space-time dimension; and(ii) there is a limiting case for the Tulley-Fisher relationship linking thespeed of light to the mass of the Universe.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "High-resolution infrared spectroscopy in the 2.3-4.6 micron region isreported for the peculiar A supergiant, single-lined spectroscopic binary HR4049. Lines from the CO fundamental and first overtone, OH fundamental, andseveral H2O vibration-rotation transitions have been observed in thenear-infrared spectrum. The spectrum of HR 4049 appears principally in emissionthrough the 3 and 4.6 micron region and in absorption in the 2 micron region.The 4.6 micron spectrum shows a rich 'forest' of emission lines. All thespectral lines observed in the 2.3-4.6 micron spectrum are shown to becircumbinary in origin. The presence of OH and H2O lines confirm theoxygen-rich nature of the circumbinary gas which is in contrast to thepreviously detected carbon-rich material. The emission and absorption lineprofiles show that the circumbinary gas is located in a thin, rotating layernear the dust disk. The properties of the dust and gas circumbinary disk andthe spectroscopic orbit yield masses for the individual stars, M_AI~0.58 Msolarand M_MV~0.34 Msolar. Gas in the disk also has an outward flow with a velocityof $\\gtrsim$ 1 km/s. The severe depletion of refractory elements but near-solarabundances of volatile elements observed in HR 4049 results from abundancewinnowing. The separation of the volatiles from the grains in the disk and thesubsequent accretion by the star are discussed. Contrary to prior reports, theHR 4049 carbon and oxygen isotopic abundances are typical AGB values:12C/13C=6^{+9}_{-4} and 16O/17O>200.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Following deep astrometric and photometric study of the cluster NGC2682(M67), we are able to accurately determine its fundamental parameters. Being anold and rich cluster, M67 is a relevant object for the analysis of the Galacticdisk evolution. M67 is well studied but the lack of a wide and deep Stromgrenphotometric study makes our results worthwhile. The brightest stars of the opencluster M67 were used as uvby-Hbeta standard stars in our studies of NGC1817and NGC2548, and the extension of the field covered, as well as the amount ofobservations, allowed to obtain the best set of Stromgren data ever publishedfor this cluster. We discuss the results of our CCD uvby-Hbetaintermediate-band photometry, covering an area of about 50'x50' down to V 19.Moreover, a complete membership segregation based on astrometric andphotometric criteria is obtained. The photometric analysis of a selected sampleof stars yields a reddening value of E(b-y)= 0.03\\pm0.03, a distance modulus ofV_0-M_V= 9.7\\pm0.2 and [Fe/H]= 0.01\\pm0.14. Through isochrone fitting we foundan age of log t= 9.6\\pm0.1 (4.2\\pm0.2 Gyr). A clump of approximately 60 starsaround V= 16, (b-y)= 0.4 could be interpreted as a population ofpre-cataclysmic variable stars (if members), or as a stream of field G-typestars placed at twice the distance of the cluster (if non-members).", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We employ the Boltzmann equation for describing hadron production from aquark-gluon plasma (QGP) in ultrarelativistic heavy-ion collisions. We proposeresonance formation in quark-antiquark scattering as the dominantmeson-production channel, which, in particular, ensures that energy isconserved in the recombination process. This, in turn, facilitates a morecontrolled extension of hadronization to low transverse momenta ($p_T$), and toaddress the experimentally observed transition from a hydrodynamic regime toconstituent quark-number scaling (CQNS). Based on input distributions forstrange and charm quarks with azimuthal asymmetries, $v_2(p_T)$, characteristicfor RHIC energies, we recover CQNS at sufficiently high $p_T$, while at low$p_T$ a scaling with transverse kinetic energy is found, reminiscent toexperiment. The dependence of the transition regime on microscopic QGPproperties, i.e. resonance widths and $Q$-values in the $q+\\bar q \\to M$process, is elucidated.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "An extension of the Standard Model by three singlet fermions with massessmaller than the electroweak scale allows to explain simultaneously neutrinooscillations, dark matter and baryon asymmetry of the Universe. We discuss theproperties of neutral leptons in this model and the ways they can be searchedfor in particle physics experiments. We establish, in particular, a lower andan upper bound on the strength of interaction of neutral leptons coming fromcosmological considerations and from the data on neutrino oscillations. Weanalyse the production of neutral leptons in the decays of different mesons andin $pp$ collisions. We study in detail decays of neutral leptons and establisha lower bound on their mass coming from existing experimental data and Big BangNucleosynthesis. We argue that the search for a specific missing energy signalin kaon decays would allow to strengthen considerably the bounds on neutralfermion couplings and to find or definitely exclude them below the kaonthreshold. To enter into cosmologically interesting parameter range for massesabove kaon mass the dedicated searches similar to CERN PS191 experiment wouldbe needed with the use of intensive proton beams. We argue that the use ofCNGS, NuMI, T2K or NuTeV beams could allow to search for singlet leptons belowcharm in a large portion of the parameter space of the nuMSM. The search ofsinglet fermions in the mass interval 2-5 GeV would require a considerableincrease of the intensity of proton accelerators or the detailed analysis ofkinematics of more than 10^{10} B-meson decays.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "A classical problem in elasticity theory involves an inhomogeneity embeddedin a material of given stress and shear moduli. The inhomogeneity is a regionof arbitrary shape whose stress and shear moduli differ from those of thesurrounding medium. In this paper we present a new, semi-analytic method forfinding the stress tensor for an infinite plate with such an inhomogeneity. Thesolution involves two conformal maps, one from the inside and the second fromthe outside of the unit circle to the inside, and respectively outside, of theinhomogeneity. The method provides a solution by matching the conformal maps onthe boundary between the inhomogeneity and the surrounding material. Thismatching converges well only for relatively mild distortions of the unit circledue to reasons which will be discussed in the article. We provide a comparisonof the present result to known previous results.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "An apparatus for producing atomic-gas Bose-Einstein condensates (BECs) of87-Rb atoms is described. The apparatus produces 87-Rb BECs in a dual-chambervacuum system that incorporates magnetic transport of trapped atoms from themagneto-optical trapping cell to the BEC production cell via the operation of aseries of overlapping magnet coils. The design, construction, and operation ofthe apparatus are described in detail. The apparatus is used to study thecreation of quantized vortices in BECs by the merging and interference ofmultiple trapped condensates. In this experiment, a single harmonic potentialwell is partitioned into three sections by an optical barrier, enabling thesimultaneous formation of three independent, uncorrelated BECs. The BECs mayeither merge together during their growth, or, for high-energy barriers, theBECs can be merged together by barrier removal after their formation. Eitherprocess may instigate vortex formation in the resulting BEC, depending on theinitially indeterminate relative phases of the condensates and the mergingrate.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Binary microlensing light curves have a variety of morphologies. Many areindistinguishable from point lens light curves. Of those that deviate from thepoint lens form, caustic crossing light curves have tended to dominateidentified binary lens events. Other distinctive signatures of binary lensesinclude significant asymmetry, multiple peaks, and repeating events. We havequantified, using high resolution simulations, the theoretically expectedrelative numbers of each type of binary lens event, based on its measurablecharacteristics. We find that a microlensing survey with current levels ofphotometric uncertainty and sampling should find at least as many non-causticcrossing binary lens events as caustic crossing events; in future surveys withmore sensitive photometry, the contribution of distinctive non-caustic crossingevents will be even greater. To try to explain why caustic crossing lightcurves appear to be so dominant among the published binary lensing events, weinvestigate the influence of several physical effects, including blending,sampling rate, and various binary populations.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "A significant fraction of Lyman Alpha (Lya) emitting galaxies (LAEs) at z>5.7 have rest-frame equivalent widths (EW) greater than ~100 Angstrom. Howeveronly a small fraction of the Lya flux produced by a galaxy is transmittedthrough the IGM, which implies intrinsic Lya EWs that are in excess of themaximum allowed for a population-II stellar population having a Salpeter massfunction. In this paper we study characteristics of the sources powering Lyaemission in high redshift galaxies. We propose a simple model for Lya emittersin which galaxies undergo a burst of very massive star formation that resultsin a large intrinsic EW, followed by a phase of population-II star formationwith a lower EW. We confront this model with a range of high redshiftobservations and find that the model is able to simultaneously describe thefollowing eight properties of the high redshift galaxy population withplausible values for parameters like the efficiency and duration of starformation: i-iv) the UV and Lya luminosity functions of LAEs at z=5.7 and 6.5,v-vi) the mean and variance of the EW distribution of Lya selected galaxies atz=5.7, vii) the EW distribution of i-drop galaxies at z~6, and viii) theobserved correlation of stellar age with EW. Our modeling suggests that theobserved anomalously large intrinsic equivalent widths require a burst of verymassive star formation lasting no more than a few to ten percent of thegalaxies star forming lifetime. This very massive star formation may indicatethe presence of population-III star formation in a few per cent of i-dropgalaxies, and in about half of the Lya selected galaxies.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present the results from simultaneous chandra and rxte observations of theX-ray bright Broad-Line Radio Galaxy (BLRG) 3C 382. The long (120 ks) exposurewith chandra HETG allows a detailed study of the soft X-ray continuum and ofthe narrow component of the Fe Kalpha line. The rxte PCA data are used to putan upper limit on the broad line component and constrain the hard X-raycontinuum. A strong soft excess below 1 keV is observed in the time-averagedHETG spectrum, which can be parameterized with a steep power law or a thermalmodel. The flux variability at low energies indicates that the origin of thesoft excess cannot be entirely ascribed to the circumnuclear diffuse emission,detected by chandra on scales of 20-30 arcsec (22-33 kpc). A narrow (sigma<90eV) Fe Kalpha line (with EW< 100 eV) is observed by the chandra HEG. Similarvalues for the line parameters are measured by the rxte PCA, suggesting thatthe contribution from a broad line component is negligible. The fact that theexposure is split into two observations taken three days apart allows us toinvestigate the spectral and temporal evolution of the source on differenttimescales. Significant flux variability associated with spectral changes isobserved on timescales of hours and days. The spectral variability is similarto that observed in radio-quiet AGN ruling out a jet-dominated origin of theX-rays.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We review the possibility that the Supersymmetric Standard Model arises fromorbifold constructions of the E_8 x E_8 Heterotic Superstring, and thephenomenological properties that such a model should have. In particular,trying to solve the discrepancy between the unification scale predicted by theHeterotic Superstring (g_{GUT}x5.27x10^{17} GeV) and the value deduced from LEPexperiments (2x10^{16} GeV), we will predict the presence at low energies ofthree families of Higgses and vector-like colour triplets. Our approach relieson the Fayet-Iliopoulos breaking, and this is also a crucial ingredient,together with having three Higgs families, to obtain in these models aninteresting pattern of fermion masses and mixing angles at the renormalizablelebel. Namely, after the gauge breaking some physical particles appear combinedwith other states, and the Yukawa couplings are modified in a well controlledway. On the other hand, dangerous flavour-changing neutral currents may appearwhen fermions of a given charge receive their mass through couplings withseveral Higgs doublets. We will address this potential problem, finding thatviable scenarios can be obtained for a reasonable light Higgs spectrum.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We report the discovery of an X-ray counterpart to the southern radio hotspotof the largest-known radio quasar 4C 74.26 (whose redshift is z=0.104). BothXMM-Newton and Chandra images reveal the same significant (10arcsec, i.e.19kpc) offset between the X-ray hotspot and the radio hotspot imaged withMERLIN. The peak of the X-ray emission may be due to synchrotron orinverse-Compton emission. If synchrotron emission, the hotspot represents thesite of particle acceleration and the offset arises from either the jetexhibiting Scheuer's `dentist's drill' effect or a fast spine having lessmomentum than the sheath surrounding it, which creates the radio hotspot. Ifthe emission arises from the inverse-Compton process, it must beinverse-Compton scattering of the CMB in a decelerating relativistic flow,implying that the jet is relativistic (Gamma >= 2) out to a distance of atleast 800kpc. Our analysis, including optical data from the LiverpoolTelescope, rules out a background AGN for the X-ray emission and confirms itsnature as a hotspot, making it the most X-ray luminous hotspot yet detected.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We introduce and study the notion of relative rigidity for pairs $(X,\\JJ)$where 1) $X$ is a hyperbolic metric space and $\\JJ$ a collection of quasiconvexsets 2) $X$ is a relatively hyperbolic group and $\\JJ$ the collection ofparabolics 3) $X$ is a higher rank symmetric space and $\\JJ$ an equivariantcollection of maximal flats Relative rigidity can roughly be described asupgrading a uniformly proper map between two such $\\JJ$'s to a quasi-isometrybetween the corresponding $X$'s.  A related notion is that of a $C$-complex which is the adaptation of a Titscomplex to this context. We prove the relative rigidity of the collection ofpairs $(X, \\JJ)$ as above. This generalises a result of Schwarz for symmetricpatterns of geodesics in hyperbolic space. We show that a uniformly proper mapinduces an isomorphism of the corresponding $C$-complexes. We also give acouple of characterizations of quasiconvexity. of subgroups of hyperbolicgroups on the way.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "This paper quantifies the information rate of multiple-input multiple-output(MIMO) systems with finite rate channel state feedback and power on/offstrategy. In power on/off strategy, a beamforming vector (beam) is eitherturned on (denoted by on-beam) with a constant power or turned off. We provethat the ratio of the optimal number of on-beams and the number of antennasconverges to a constant for a given signal-to-noise ratio (SNR) when the numberof transmit and receive antennas approaches infinity simultaneously and whenbeamforming is perfect. Based on this result, a near optimal strategy, i.e.,power on/off strategy with a constant number of on-beams, is discussed. Forsuch a strategy, we propose the power efficiency factor to quantify the effectof imperfect beamforming. A formula is proposed to compute the maximum powerefficiency factor achievable given a feedback rate. The information rate of theoverall MIMO system can be approximated by combining the asymptotic results andthe formula for power efficiency factor. Simulations show that thisapproximation is accurate for all SNR regimes.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "A synfire chain is a simple neural network model which can propagate stablesynchronous spikes called a pulse packet and widely researched. However howsynfire chains coexist in one network remains to be elucidated. We have studiedthe activity of a layered associative network of Leaky Integrate-and-Fireneurons in which connection we embed memory patterns by the Hebbian Learning.We analyzed their activity by the Fokker-Planck method. In our previous report,when a half of neurons belongs to each memory pattern (memory pattern rate$F=0.5$), the temporal profiles of the network activity is split intotemporally clustered groups called sublattices under certain input conditions.In this study, we show that when the network is sparsely connected ($F<0.5$),synchronous firings of the memory pattern are promoted. On the contrary, thedensely connected network ($F>0.5$) inhibit synchronous firings. The sparsenessand denseness also effect the basin of attraction and the storage capacity ofthe embedded memory patterns. We show that the sparsely(densely) connectednetworks enlarge(shrink) the basion of attraction and increase(decrease) thestorage capacity.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We extend previous analyses of the supersymmetric loop correction to theneutral Higgs couplings to include the coupling $\\chi^{+}_j \\chi^{-}_kH^{0}_l$.The analysis completes the previous analyses where similar corrections werecomputed for the $\\bar{\\tau} \\tau H^{0}_l$, $\\bar{b} b H^{0}_l$, $\\bar{c} cH^{0}_l$ and for $\\bar{t} t H^{0}_l$ couplings within the minimalsupersymmetric standard model. The effective one loop Lagrangian is thenapplied to the computation of the neutral Higgs decays. The sizes of thesupersymmetric loop corrections of the neutral Higgs decay widths into$\\chi^{+}_i \\chi^{-}_j$ ($i=1,2$; $j=1,2$) are investigated and thesupersymmetric loop correction is found to be in the range of $7\\sim15%$ insignificant regions of the parameter space. By including the loop correctionsof the other decay channels $\\bar{b} b$, $\\bar{t} t$, $\\bar{\\tau} \\tau$,$\\bar{c} c$, and $\\chi^0_i \\chi^0_j$ ($i=1-4$; $j=1-4$), the corrections tobranching ratios for $H^{0}_l\\to \\chi^{+}_i \\chi^{-}_j$ can reach as high as40%.  The effects of CP phases on the branching ratio are also investigated.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "In a number of physically important cases, the nonholonomically(nonintegrable) constrained Ricci flows can be modelled by exact solutions ofEinstein equations with nonhomogeneous (anisotropic) cosmological constants. Wedevelop two geometric methods for constructing such solutions: The firstapproach applies the formalism of nonholonomic frame deformations when thegravitational evolution and field equations transform into systems of nonlinearpartial differential equations which can be integrated in general form. Thesecond approach develops a general scheme when one (two) parameter families ofexact solutions are defined by any source-free solutions of Einstein'sequations with one (two) Killing vector field(s). A successive iterationprocedure results in a class of solutions characterized by an infinite numberof parameters for a non-Abelian group involving arbitrary functions on onevariable. We also consider nonlinear superpositions of some mentioned classesof solutions in order to construct more general integral varieties of the Ricciflow and Einstein equations depending on infinite number of parameters andthree/ four coordinates on four/ five dimensional (semi) Riemannian spaces.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Many ambitious experiments have been proposed to constrain dark energy anddetect its evolution. At present, observational constraints are consistent witha cosmological constant and there is no firm evidence for any evolution in thedark energy equation of state w. In this paper, we pose the following question:suppose that future dark energy surveys constrain w at low redshift to beconsistent with -1 to a percent level accuracy, what are the implications formodels of dynamical dark energy? We investigate this problem in amodel-independent way by following quintessence field trajectories in `energy'phase-space. Attractor dynamics in this phase-space leads to two classes ofacceptable models: 1) models with flat potentials, i.e. an effectivecosmological constant, and 2) models with potentials that suddenly flatten witha characteristic kink. The prospect of further constraining the second class ofmodels from distance measurements and fluctuation growth rates at low redshift(z<3) seems poor. However, in some models of this second class, the dark energymakes a significant contribution to the total energy density at high redshift.Such models can be further constrained from observation of the cosmic microwavebackground anisotropies and from primordial nucleosynthesis. It is possible,therefore, to construct models in which the dark energy at high redshift causesobservable effects, even if future dark energy surveys constrain w at lowredshift to be consistent with -1 to high precision.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Since the discovery of the first L dwarf 19 years ago and the discovery ofthe first T dwarf 7 years after that, we have amassed a large list of theseobjects, now numbering almost six hundred. Despite making headway inunderstanding the physical chemistry of their atmospheres, some importantissues remain unexplained. Three of these are the subject of this paper: (1)What is the role of \"second parameters\" such as gravity and metallicity inshaping the emergent spectra of L and T dwarfs? Can we establish a robustclassification scheme so that objects with unusual values of log(g) or [M/H],unusual dust content, or unresolved binarity are easily recognized? (2) Whichphysical processes drive the unusual behavior at the L/T transition? Whichobservations can be obtained to better confine the problem? (3) What willobjects cooler than T8 look like? How will we know a Y dwarf when we firstobserve one?", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We define Poincar\\'e series associated to a toric or analytically irreduciblequasi-ordinary hypersurface singularity, (S,0), by a finite sequence ofmonomial valuations, such that at least one of them is centered at the origin0. This involves the definition of a multi-graded ring associated to theanalytic algebra of the singularity by the sequence of valuations. We provethat the Poincar\\'e series is a rational function with integer coefficients,which can be defined also as an integral with respect of the Eulercharacteristic, over the projectivization of the analytic algebra of thesingularity, of a function defined by the valuations. In particular, thePoincar\\'e series associated to the set of divisorial valuations associated tothe essential divisors, considered both over the singular locus and over thepoint 0, is an analytic invariant of the singularity. In the quasi-ordinaryhypersurface case we prove that this Poincar\\'e series determines and it isdetermined by the normalized sequence of characteristic monomials. Thesemonomials in the analytic case define a complete invariant of the embeddedtopological type of the hypersurface singularity.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present analytical and numerical studies of phase-coherent dynamics ofintrinsically localized excitations (breathers) in a system of two weaklycoupled nonlinear oscillator chains. We show that there are two qualitativelydifferent dynamical regimes of the coupled breathers, either immovable orslowly-moving: the periodic transverse translation (wandering) of low-amplitudebreather between the chains, and the one-chain-localization of high-amplitudebreather. These two modes of coupled nonlinear excitations, which involve largenumber of anharmonic oscillators, can be mapped onto two solutions of a singlependulum equation, detached by a separatrix mode. We also study two-chainbreathers, which can be considered as bound states of discrete breathers withdifferent symmetry and center locations in the coupled chains, and bifurcationof the anti-phase two-chain breather into the one-chain one. Delocalizingtransition of 1D breather in 2D system of a large number of parallel couplednonlinear chains is described, in which the breather, initially excited in agiven chain, abruptly spreads its vibration energy in the whole 2D system upondecreasing breather frequency or amplitude below the threshold one. Thethreshold breather frequency is above the cut off phonon frequency in 2Dsystem, and the threshold breather amplitude scales as square root of theinter-chain coupling constant. Delocalizing transition of discrete vibrationalbreather in 2D and 3D systems of coupled nonlinear chains has an analogy withdelocalizing transition for Bose-Einstein condensates in 2D and 3D opticallattices.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The vacuum dependence on boundary conditions in quantum field theories isanalysed from a very general viewpoint. From this perspective therenormalization prescriptions not only imply the renormalization of thecouplings of the theory in the bulk but also the appearance of a flow in thespace of boundary conditions. For regular boundaries this flow has a largevariety of fixed points and no cyclic orbit. The family of fixed pointsincludes Neumann and Dirichlet boundary conditions. In one-dimensional fieldtheories pseudoperiodic and quasiperiodic boundary conditions are also RG fixedpoints. Under these conditions massless bosonic free field theories areconformally invariant. Among all fixed points only Neumann boundary conditionsare infrared stable fixed points. All other conformal invariant boundaryconditions become unstable under some relevant perturbations. In finite volumeswe analyse the dependence of the vacuum energy along the trajectories of therenormalization group flow providing an interesting framework for dark energyevolution. On the contrary, the renormalization group flow on the boundary doesnot affect the leading behaviour of the entanglement entropy of the vacuum inone-dimensional conformally invariant bosonic theories.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "In this paper, it is shown that the cosmological model that was introduced ina sequence of three earlier papers under the title, A Dust Universe Solution tothe Dark Energy Problem, can be used to resolve the problem of the greatmismatch of numerical values between dark energy from cosmology and zero pointenergy from quantum theory. It is shown that, if the zero point energies forthe cosmic microwave background and for all the rest of the universe that isnot cosmic microwave background are introduced into this model as two entities,their separate values appear within this theory in the form of a numericaldifference. It is this difference that gives the numerical value for the zeropoint value of Einstein's dark energy density. Consequently, although the twozero point energies may be large, their difference can give the known smalldark energy value from cosmology for dark energy density. Issues relating tointerpretation, calculation and measurement associated with this result and aninterpretation of dark energy as a measure of polarisation of the vacuum arediscussed. In the first appendix to this paper, problems associated with thestandard model of cosmology are solved by redefining temperature in the dustuniverse model. In the second appendix of this paper, an examination of thedark matter problem in relation to a general relativistic generalisation ofNewton's inverse square law is undertaken. In the third appendix to this paper,the formalism is used to derive a formula that gives a possible value for themass of the universe in terms of Newton's gravitation constant, Einstein'sLambda and the velocity of light. All three appendices have their own detailedabstracts.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "By analyzing the relationships between a socioeconomical system modeledthrough evolutionary game theory and a physical system modeled through quantummechanics we show how although both systems are described through two theoriesapparently different both are analogous and thus exactly equivalents. Theextensions of quantum mechanics to statistical physics and information theorylet us use some of their definitions for the best understanding of the behaviorof economics and biology. The quantum analogue of the replicator dynamics isthe von Neumann equation. A system in where all its members are in Nashequilibrium is equivalent to a system in a maximum entropy state. Nature is agame in where its players compete for a common welfare and the equilibrium ofthe system that they are members. They act as a whole besides individuals likethey obey a rule in where they prefer to work for the welfare of the collectivebesides the individual welfare.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The calculation of conserved charges of black holes is a rich problem, forwhich many methods are known. Until recently, there was some controversy on theproper definition of conserved charges in asymptotically anti-de Sitter (AdS)spaces in arbitrary dimensions. This paper provides a systematic and explicitHamiltonian derivation of the energy and the angular momenta of bothasymptotically flat and asymptotically AdS spacetimes in any dimension D biggeror equal to 4. This requires as a first step a precise determination of theasymptotic conditions of the metric and of its conjugate momentum. Theseconditions happen to be achieved in ellipsoidal coordinates adapted to therotating solutions.The asymptotic symmetry algebra is found to be isomorphiceither to the Poincare algebra or to the so(D-1, 2) algebra, as expected. Inthe asymptotically flat case, the boundary conditions involve a generalizationof the parity conditions, introduced by Regge and Teitelboim, which arenecessary to make the angular momenta finite. The charges are explicitlycomputed for Kerr and Kerr-AdS black holes for arbitrary D and they are shownto be in agreement with thermodynamical arguments.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We report the discovery of one of the most powerful sunquakes detected todate, produced by an X1.2-class solar flare in active region 10720 on 2005January 15. We used helioseismic holography to image the source of seismicwaves emitted into the solar interior from the site of the flare. Acousticegression power maps at 3 and 6 mHz with a 2 mHz bandpass reveal a compactacoustic source strongly correlated with impulsive hard X-ray andvisible-continuum emission along the penumbral neutral line separating the twomajor opposing umbrae in the $\\delta$-configuration sunspot that predominatesAR10720. The acoustic emission signatures were directly aligned with both hardX-ray and visible continuum emission that emanated during the flare. Thevisible continuum emission is estimated at $2.0 \\times 10^{23}$ J,approximately 500 times the seismic emission of $\\sim 4 \\times 10^{20}$ J. Theflare of 2005 January 15 exhibits the same close spatial alignment between thesources of the seismic emission and impulsive visible continuum emission asprevious flares, reinforcing the hypothesis that the acoustic emission may bedriven by heating of the low photosphere. However, it is a major exception inthat there was no signature to indicate the inclusion of protons in theparticle beams thought to supply the energy radiated by the flare. Thecontinued strong coincidence between the sources of seismic emission andimpulsive visible continuum emission in the case of a proton-deficientwhite-light flare lends substantial support to the ``back -- warming''hypothesis, that the low photosphere is significantly heated by intense Balmerand Paschen continuum-edge radiation from the overlying chromosphere inwhite-light flares.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We construct a commutative algebra A_x of difference operators in R^p,depending on p+3 real parameters which is diagonalized by the multivariableRacah polynomials R_p(n;x) considered by Tratnik [27]. It is shown that forspecific values of the variables x=(x_1,x_2,...,x_p) there is a hidden dualitybetween n and x. Analytic continuation allows us to construct anothercommutative algebra A_n in the variables n=(n_1,n_2,...,n_p) which is alsodiagonalized by R_p(n;x). Thus R_p(n;x) solve a multivariable discretebispectral problem in the sense of Duistermaat and Grunbaum [8]. Since a changeof the variables and the parameters in the Racah polynomials gives themultivariable Wilson polynomials [26], this change of variables and parametersin A_x and A_n leads to bispectral commutative algebras for the multivariableWilson polynomials.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "A recent advance in improving the spatial resolution of magnetic forcemicroscopy (MFM) uses as sensor tips carbon nanotubes grown at the apex ofconventional silicon cantilever pyramids and coated with a thin ferromagneticlayer. Magnetic images of high density vertically recorded media using thesetips exhibit a doubling of the spatial frequency under some conditions. Here wedemonstrate that this spatial frequency doubling is due to the switching of themoment direction of the nanotube tip. This results in a signal which isproportional to the absolute value of the signal normally observed in MFM. Ourmodeling indicates that a significant fraction of the tip volume is involved inthe observed switching, and that it should be possible to image very high bitdensities with nanotube magnetic force sensors.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We consider normalizers of an irreducible inclusion $N\\subseteq M$ of$\\mathrm{II}_1$ factors. In the infinite index setting an inclusion$uNu^*\\subseteq N$ can be strict, forcing us to also investigate the semigroupof one-sided normalizers. We relate these normalizers of $N$ in $M$ toprojections in the basic construction and show that every trace one projectionin the relative commutant $N'\\cap < M,e_N>$ is of the form $u^*e_Nu$ for someunitary $u\\in M$ with $uNu^*\\subseteq N$. This enables us to identify thenormalizers and the algebras they generate in several situations. In particulareach normalizer of a tensor product of irreducible subfactors is a tensorproduct of normalizers modulo a unitary. We also examine normalizers ofirreducible subfactors arising from subgroup--group inclusions $H\\subseteq G$.Here the normalizers are the normalizing group elements modulo a unitary from$L(H)$. We are also able to identify the finite trace $L(H)$-bimodules in$\\ell^2(G)$ as double cosets which are also finite unions of left cosets.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We derive the microcanonical partition function of the ideal relativisticquantum gas of spinless bosons in a quantum field framework as an expansionover fixed multiplicities. Our calculation generalizes well known expressionsin literature in that it does not introduce any large volume approximation andit is valid at any volume. We discuss the issues concerned with the definitionof the microcanonical ensemble for a free quantum field at volumes comparablewith the Compton wavelength and provide a consistent prescription ofcalculating the microcanonical partition function, which is finite at finitevolume and yielding the correct thermodynamic limit. Besides an immaterialoverall factor, the obtained expression turns out to be the same as in thenon-relativistic multi-particle approach. This work is introductory to derivethe most general expression of the microcanonical partition function fixing themaximal set of observables of the Poincare' group.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Colliding winds of massive stars in binary systems are considered ascandidate sites of high-energy non-thermal photon emission. They are alreadyamong the suggested counterparts for a few individual unidentified EGRETsources, but may constitute a detectable source population for the GLASTobservatory. The present work investigates such population study of massivecolliding wind systems at high-energy gamma-rays. Based on the recent detailedmodel (Reimer et al. 2006) for non-thermal photon production in prime candidatesystems, we unveil the expected characteristics of this source class in theobservables accessible at LAT energies. Combining the broadband emission modelwith the presently cataloged distribution of such systems and their individualparameters allows us to conclude on the expected maximum number ofLAT-detections among massive stars in colliding wind binary systems.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We examine Gaussian-basis Monte Carlo method (GBMC) introduced by Corney andDrummond. This method is based on an expansion of the density-matrix operatorrho by means of the coherent Gaussian-type operator basis Lambda and does notsuffer from the minus sign problem. The original method, however, often failsin reproducing the true ground state and causes systematic errors of calculatedphysical quantities because the samples are often trapped in some metastable orsymmetry broken states. To overcome this difficulty, we combine thequantum-number projection scheme proposed by Assaad, Werner, Corboz, Gull andTroyer in conjunction with the importance sampling of the original GBMC method.This improvement allows us to carry out the importance sampling in thequantum-number-projected phase-space. Some comparisons with the previousquantum-number projection scheme indicate that, in our method, the convergencewith the ground state is accelerated, which makes it possible to extend theapplicability and widen the range of tractable parameters in the GBMC method.The present scheme offers an efficient practical way of computation forstrongly correlated electron systems beyond the range of system sizes,interaction strengths and lattice structures tractable by other computationalmethods such as the quantum Monte Carlo method.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Hundreds of substellar companions to solar-type stars will be discovered withthe Kepler satellite. Kepler's extreme photometric precision gives access tolow-amplitude stellar variability contributed by a variety of physicalprocesses. We discuss in detail the periodic flux modulations arising from thetidal force on the star due to a substellar companion. An analytic expressionfor the variability is derived in the equilibrium-tide approximation. Wedemonstrate analytically and through numerical solutions of the linear,nonadiabatic stellar oscillation equations that the equilibrium-tide formulaworks extremely well for stars of mass <1.4 Msun with thick surface convectionzones. More massive stars with largely radiative envelopes do not conform tothe equilibrium-tide approximation and can exhibit flux variations $\\ga$10times larger than naive estimates. Over the full range of stellar massesconsidered, we treat the oscillatory response of the convection zone byadapting a prescription that A. J. Brickhill developed for pulsating whitedwarfs. Compared to other sources of periodic variability, the ellipsoidallightcurve has a distinct dependence on time and system parameters. We suggestthat ellipsoidal oscillations induced by giant planets may be detectable fromas many as ~100 of the 10^5 Kepler target stars. (Abridged)", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "In papers I and II in this series, we presented hydrodynamical simulations ofjet models with parameters representative of the symbiotic system MWC 560.These were simulations of a pulsed, initially underdense jet in a high densityambient medium. Since the pulsed emission of the jet creates internal shocksand since the jet velocity is very high, the jet bow shock and the internalshocks are heated to high temperatures and should therefore emit X-rayradiation. In this paper, we investigate in detail the X-ray properties of thejets in our models. We have focused our study on the total X-ray luminosity andits temporal variability, the resulting spectra and the spatial distribution ofthe emission. Temperature and density maps from our hydrodynamical simulationswith radiative cooling presented in the second paper are used together withemissivities calculated with the atomic database ATOMDB. The jets in our modelsshow extended and variable X-ray emission which can be characterized as a sumof hot and warm components with temperatures that are consistent withobservations of CH Cyg and R Aqr. The X-ray spectra of our model jets showemission line features which correspond to observed features in the spectra ofCH Cyg. The innermost parts of our pulsed jets show iron line emission in the6.4 - 6.7 keV range which may explain such emission from the central source inR Aqr. We conclude that MWC 560 should be detectable with Chandra orXMM-Newton, and such X-ray observations will provide crucial for understandingjets in symbiotic stars.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We study theoretically the Josephson effect in d-wave superconductor /diffusive normal metal /insulator/ diffusive normal metal/ d-wavesuperconductor (D/DN/I/DN/D) junctions. This model is aimed to describepractical junctions in high-$T_C$ cuprate superconductors, in which the productof the critical Josephson current ($I_C$) and the normal state resistance ($R$)(the so-called $I_{\\rm C}R$ product) is very small compared to the predictionof the standard theory. We show that the $I_{\\rm C}R$ product in D/DN/I/DN/Djunctions can be much smaller than that in d-wave superconductor / insulator /d-wave superconductor junctions and formulate the conditions necessary toachieve large $I_{\\rm C}R$ product in D/DN/I/DN/D junctions. The proposedtheory describes the behavior of $I_{\\rm C}R$ products quantitatively inhigh-$T_{\\rm C}$ cuprate junctions.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The object NGC6908 was once thought to be simply a surface-brightnessenhancement in the eastern spiral arm of the nearby spiral galaxy NGC6907.Based on an examination of near-infrared imaging, the object is shown in factto be a lenticular S0(6/7) galaxy hidden in the optical glare of the disk andspiral structure of the larger galaxy. New radial velocities of NGC6908(3,060+/-16 (emission); 3,113+/-73 km/s (absorption)) have been obtained at theBaade 6.5m and the duPont 2.5m telescopes at Las Campanas, Chile placingNGC6908 at the same expansion-velocity distance as NGC6907 (3,190+/-5 km/s),eliminating the possibility of a purely chance line-of-sight coincidence. Theonce-enigmatic asymmetries in the disk and outer spiral structure of NGC6907are now explained as being due to an advanced merger event. Newly discoveredtails and debris in the outer reaches of this galaxy further support the mergerscenario for this system. This pair of galaxies is a rather striking example oftwo objects discovered over 100 years ago, whose true nature was lost untilmodern detectors operating at infrared wavelengths gave us a new(high-contrast) look. Other examples of embedded merger remnants may alsoreveal themselves in the growing samples of near-infrared imaging of nearbygalaxies; and a pilot study does reveal several other promising candidates forfollow-up observations.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "GEMS and GOODS fields were examined to z~1.4 for galaxy interactions andmergers. The basic morphologies are familiar: antennae with long tidal tails,tidal dwarfs, and merged cores; M51-type galaxies with disk spirals and tidalarm companions; early-type galaxies with diffuse plumes; equal-massgrazing-collisions; and thick J-shaped tails beaded with star formation anddouble cores. One type is not common locally and is apparently a looseassemblage of smaller galaxies. Photometric measurements were made of the tailsand clumps, and physical sizes were determined assuming photometric redshifts.Antennae tails are a factor of ~3 smaller in GEMS and GOODS systems compared tolocal antennae; their disks are a factor of ~2 smaller than locally. Collisionsamong early type galaxies generally show no fine structure in their tails,indicating that stellar debris is usually not unstable. One exception has a5x10**9 Msun smooth red clump that could be a pure stellar condensation. Mosttidal dwarfs are blue and probably form by gravitational instabilities in thegas. One tidal dwarf looks like it existed previously and was incorporated intothe arm tip by tidal forces. The star-forming regions in tidal arms are 10 to1000 times more massive than star complexes in local galaxies, although theirseparations are about the same. If they all form by gravitationalinstabilities, then the gaseous velocity dispersions in interacting galaxieshave to be larger than in local galaxies by a factor of ~5 or more; the gascolumn densities have to be larger by the square of this factor.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present the fourth edition of the Sloan Digital Sky Survey (SDSS) QuasarCatalog. The catalog contains 77,429 objects; this is an increase of over30,000 entries since the previous edition. The catalog consists of the objectsin the SDSS Fifth Data Release that have luminosities larger than M_i = -22.0(in a cosmology with H_0 = 70 km/s/Mpc, Omega_M = 0.3, and Omega_Lambda = 0.7)have at least one emission line with FWHM larger than 1000 km/s, or haveinteresting/complex absorption features, are fainter than i=15.0, and havehighly reliable redshifts. The area covered by the catalog is 5740 sq. deg. Thequasar redshifts range from 0.08 to 5.41, with a median value of 1.48; thecatalog includes 891 quasars at redshifts greater than four, of which 36 are atredshifts greater than five. Approximately half of the catalog quasars have i <19; nearly all have i < 21. For each object the catalog presents positionsaccurate to better than 0.2 arcsec. rms per coordinate, five-band (ugriz)CCD-based photometry with typical accuracy of 0.03 mag, and information on themorphology and selection method. The catalog also contains basic radio,near-infrared, and X-ray emission properties of the quasars, when available,from other large-area surveys. The calibrated digital spectra cover thewavelength region 3800--9200A at a spectral resolution of ~2000. The spectracan be retrieved from the public database using the information provided in thecatalog. The average SDSS colors of quasars as a function of redshift, derivedfrom the catalog entries, are presented in tabular form. Approximately 96% ofthe objects in the catalog were discovered by the SDSS.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We study to what extent wormholes can mimic the observational features ofblack holes. It is surprisingly found that many features that could be thoughtof as ``characteristic'' of a black hole (endowed with an event horizon) can beclosely mimicked by a globally static wormhole, having no event horizon. Thisis the case for: the apparently irreversible accretion of matter down a hole,no-hair properties, quasi-normal-mode ringing, and even the dissipativeproperties of black hole horizons, such as a finite surface resistivity equalto 377 Ohms. The only way to distinguish the two geometries on anobservationally reasonable time scale would be through the detection ofHawking's radiation, which is, however, too weak to be of practical relevancefor astrophysical black holes. We point out the existence of an interestingspectrum of quantum microstates trapped in the throat of a wormhole which couldbe relevant for storing the information ``lost'' during a gravitationalcollapse.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The network of resonant bar detectors of gravitational waves resumedcoordinated observations within the International Gravitational EventCollaboration (IGEC-2). Four detectors are taking part in this collaboration:ALLEGRO, AURIGA, EXPLORER and NAUTILUS. We present here the results of thesearch for gravitational wave bursts over 6 months during 2005, when IGEC-2 wasthe only gravitational wave observatory in operation. The network data analysisimplemented is based on a time coincidence search among AURIGA, EXPLORER andNAUTILUS, keeping the data from ALLEGRO for follow-up studies. With respect tothe previous IGEC 1997-2000 observations, the amplitude sensitivity of thedetectors to bursts improved by a factor about 3 and the sensitivity bandwidthsare wider, so that the data analysis was tuned considering a larger class ofdetectable waveforms. Thanks to the higher duty cycles of the single detectors,we decided to focus the analysis on three-fold observation, so to ensure theidentification of any single candidate of gravitational waves (gw) with highstatistical confidence. The achieved false detection rate is as low as 1 percentury. No candidates were found.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "High resolution molecular line observations of CS, HCO+, C18O and N2H+ wereobtained toward the starless globule FeSt 1-457 in order to investigate itskinematics and chemistry. The HCO+ and CS spectra show clear self-reversed andasymmetric profiles across the face of the globule. The sense of the observedasymmetry is indicative of the global presence of expansion motions in theouter layers of the globule. These motions appear to be subsonic andsignificantly below the escape velocity of the globule. Comparison of ourobservations with near-infrared extinction data indicate that the globule isgravitationally bound. Taken together these considerations lead us to suggestthat the observed expansion has its origin in an oscillatory motion of theouter layers of the globule which itself is likely in a quasi-stable state nearhydrostatic equilibrium. Analysis of the observed linewidths of CO and N2H+confirm that thermal pressure is the dominant component of the cloud's internalsupport. A simple calculation suggests that the dominant mode of pulsationwould be an l = 2 mode with a period of 0.3 Myr. Deformation of the globule dueto the large amplitude l = 2 oscillation may be responsible for thedouble-peaked structure of the core detected in high resolution extinctionmaps. Detailed comparison of the molecular-line observations and extinctiondata provides evidence for significant depletion of C18O and perhaps HCO+ whileN2H+ may be undepleted to a cloud depth of about 40 magnitudes of visualextinction.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Ordinal regression is an important type of learning, which has properties ofboth classification and regression. Here we describe a simple and effectiveapproach to adapt a traditional neural network to learn ordinal categories. Ourapproach is a generalization of the perceptron method for ordinal regression.On several benchmark datasets, our method (NNRank) outperforms a neural networkclassification method. Compared with the ordinal regression methods usingGaussian processes and support vector machines, NNRank achieves comparableperformance. Moreover, NNRank has the advantages of traditional neuralnetworks: learning in both online and batch modes, handling very large trainingdatasets, and making rapid predictions. These features make NNRank a useful andcomplementary tool for large-scale data processing tasks such as informationretrieval, web page ranking, collaborative filtering, and protein ranking inBioinformatics.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "In this article, we report the synthesis, magneto transport features, andmagnetization of polycrystalline La2/3Ca1/3MnO3:Agx/Inx composites with x = 0,0.1, 0.2, 0.3 and 0.4. In case of Ag the temperature coefficient of resistance(TCR) near ferromagnetic (FM) transition enhances significantly with additionof Ag. The FM transition temperature (TFM) is also increased slightly with Agdoping. Magneto-transport measurements revealed that magneto-resistance (MR) isfound to be maximum near TFM. Very sharp TCR is seen near TFM with highestvalue of up to 15 % for Ag (0.4) sample, which is an order of magnitude higherthan as for pristine sample and is the best value yet reported for anypolycrystalline LCMO compound. Increased TCR, TFM and significant above roomtemperature MR of La2/3Ca1/3MnO3:Agx composites is explained on the basis ofimproved grains size. Interestingly the La2/3Ca1/3MnO3:Inx composites behavedexactly in opposite way resulting in decreased TFM, and TCR compared topristine LCMO compound. In fact the grains morphology of LCMO:Inx composites isseen inferior to pristine LCMO which is opposite to the LCMO:Agx case.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We calculate angle-resolved above-threshold ionization spectra for diatomicmolecules in linearly polarized laser fields, employing the strong-fieldapproximation. The interference structure resulting from the individualcontributions of the different scattering scenarios is discussed in detail,with respect to the dependence on the internuclear distance and molecularorientation. We show that, in general, the contributions from the processes inwhich the electron is freed at one center and rescatters off the other obscurethe interference maxima and minima obtained from single-center processes.However, around the boundary of the energy regions for which rescattering has aclassical counterpart, such processes play a negligible role and very clearinterference patterns are observed. In such energy regions, one is able toinfer the internuclear distance from the energy difference between adjacentinterference minima.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We discuss Casimir effect of a massless, minimally coupled scalar field in a6D warped flux compactification model and its implications for the hierarchyand cosmological constant problems, which are longstanding puzzles inphenomenology and cosmology. Due to the scale invariance of the backgroundtheory, the 4D effective theory contains a volume modulus. To stabilize themodulus, we consider one-loop corrections to the effective potential by theCasimir effect. The one-loop effective potential for the volume modulus has aform which is very similar to Coleman-Weinberg potential. We evaluatecoefficients appearing in the effective potential by employing zeta functionregularization and heat kernel analysis. The volume modulus is stabilized forsmaller degrees of warping, below a critical value, which depends on deficitangle of the reference brane. After stabilizing the modulus, it is possible toobtain observed values of the mass ratio between the fundamental energy scalesand a tiny effective cosmological constant (though its sign is negative). Thedegree of warping should be tuned to be close to the critical value, not asseverely as the original fine-tuning.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The critical behavior of the contact process in disordered and periodicbinary 2d-lattices is investigated numerically by means of Monte Carlosimulations as well as via an analytical approximation and standard mean fieldtheory. Phase-separation lines calculated numerically are found to agree wellwith analytical predictions around the homogeneous point. For the disorderedcase, values of static scaling exponents obtained via quasi-stationarysimulations are found to change with disorder strength. In particular, thefinite-size scaling exponent of the density of infected sites approaches avalue consistent with the existence of an infinite-randomness fixed point asconjectured before for the 2d disordered CP. At the same time, both dynamicaland static scaling exponents are found to coincide with the values establishedfor the homogeneous case thus confirming that the contact process in aheterogeneous environment belongs to the directed percolation universalityclass.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We recently proposed an empirical approach for the Landau-Pomeranchuk-Migdal(LPM) effects in photon emission from the quark gluon plasma as a function ofphoton mass. This approach was based on Generalized Emission Functions (GEF)for photon emission, derived at a fixed temperature and strong couplingconstant. In the present work, we have extended the LPM calculations forseveral temperatures and strong coupling strengths. The integral equations for(${\\bf \\tilde{f}(\\tilde{p}_\\perp)}$) and ($\\tilde{g}({\\bf \\tilde{p}_\\perp})$)are solved by the iterations method for the variable set\\{$p_0,q_0,Q^2,T,\\alpha_s$\\}, considering bremsstrahlung and $\\bf aws$processes. We generalize the dynamical scaling variables, $x_T$, $x_L$, forbremsstrahlung and {\\bf aws} processes which are now functions of variables$p_0,q_0,Q^2,T,\\alpha_s$. The GEF introduced earlier, $g^b_T$, $g^a_T$,$g^b_L$, $g^a_L$, are also generalized for any temperatures and couplingstrengths. From this, the imaginary part of the photon polarization tensor as afunction of photon mass and energy can be calculated as a one dimensionalintegral over these GEF and parton distribution functions in the plasma.However, for phenomenological studies of experimental data, one needs a simpleempirical formula without involving parton momentum integrations. Therefore, wepresent a phenomenological formula for imaginary photon polarization tensor asa function of \\{$q_0,Q^2,T,\\alpha_s$\\} that includes bremsstrahlung and $\\bfaws$ mechanisms along with LPM effects.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Disordered systems present multifractal properties at criticality. Inparticular, as discovered by Ludwig (A.W.W. Ludwig, Nucl. Phys. B 330, 639(1990)) on the case of diluted two-dimensional Potts model, the moments$\\bar{\\rho^q(r)}$ of the local order parameter $\\rho(r)$ scale with a set$x(q)$ of non-trivial exponents $x(q) \\neq q x(1)$. In this paper, we revisitthese ideas to incorporate more recent findings: (i) whenever a multifractalmeasure $w(r)$ normalized over space $ \\sum_r w(r)=1$ occurs in a randomsystem, it is crucial to distinguish between the typical values and thedisorder averaged values of the generalized moments $Y_q =\\sum_r w^q(r)$, sincethey may scale with different generalized dimensions $D(q)$ and $\\tilde D(q)$(ii) as discovered by Wiseman and Domany (S. Wiseman and E. Domany, Phys Rev E{\\bf 52}, 3469 (1995)), the presence of an infinite correlation length inducesa lack of self-averaging at critical points for thermodynamic observables, inparticular for the order parameter. After this general discussion valid for anyrandom critical point, we apply these ideas to random polymer models that canbe studied numerically for large sizes and good statistics over the samples. Westudy the bidimensional wetting or the Poland-Scheraga DNA model with loopexponent $c=1.5$ (marginal disorder) and $c=1.75$ (relevant disorder). Finally,we argue that the presence of finite Griffiths ordered clusters at criticalitydetermines the asymptotic value $x(q \\to \\infty) =d$ and the minimal value $\\alpha_{min}=D(q \\to \\infty)=d-x(1) $ of the typical multifractal spectrum$f(\\alpha)$.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "This thesis provides a partial answer to a question posed by Greg Kuperbergin q-alg/9712003 and again by Justin Roberts as problem 12.18 in \"Problems oninvariants of knots and 3-manifolds\", math.GT/0406190, essentially: \"Can onedescribe the category of representations of the quantum group U_q(sl_n)(thought of as a spherical category) via generators and relations?\"  For each n \\geq 0, I define a certain tensor category of trivalent graphs,modulo isotopy, and construct a functor from this category onto (a fullsubcategory of) the category of representations of the quantum group U_q(sl_n).One would like to describe completely the kernel of this functor, by providinggenerators. The resulting quotient of the diagrammatic category would then be acategory equivalent to the representation category of U_q(sl_n).  I make significant progress towards this, describing certain generators ofthe kernel, and some obstructions to further elements. It remains a conjecturethat these relations generate the kernel. My results extend those ofq-alg/9712003, MR1659228, math.QA/0310143 and math.GT/0506403.  The argument is essentially by constructing a diagrammatic version of theforgetful functor coming from the inclusion of U_q(sl_{n-1}) in U_q(sl_n}. Weknow this functor is faithful, so a diagram is in the kernel for n exactly ifits image under the diagrammatic forgetful functor is in the kernel for n-1.This allows us to perform inductive calculations, both establishing families ofelements of the kernel, and finding obstructions.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "In this article we calculate the surface phase diagram of a two-dimensionalhard-rod fluid confined between two hard lines. In a first stage we study thesemi-infinite system consisting of an isotropic fluid in contact with a singlehard line. We have found complete wetting by the columnar phase at thewall-isotropic fluid interface. When the fluid is confined between two hardwalls, capillary columnar ordering occurs via a first-order phase transition.For higher chemical potentials the system exhibits layering transitions evenfor very narrow slits (near the one-dimensional limit). The theoretical modelused was a density-functional theory based on the Fundamental-MeasureFunctional applied to a fluid of hard rectangles in the restricted-orientationapproximation (Zwanzig model). The results presented here can be checkedexperimentally in two-dimensional granular media made of rods, where verticalmotions induced by an external source and excluded volume interactions betweenthe grains allow the system to explore those stationary states whichentropically maximize packing configurations. We claim that some of the surfacephenomena found here can be present in two-dimensional granular-media fluids.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present an examination of the kinematics and stellar populations of asample of 3 Brightest Group Galaxies (BGGs) and 3 Brightest Cluster Galaxies(BCGs) in X-ray groups and clusters. We have obtained high signal-to-noiseGemini/GMOS (Gemini South Multi-Object Spectrograph) long-slit spectra of thesegalaxies and use Lick indices to determine ages, metallicities andalpha-element abundance ratios out to at least their effective radii. We findthat the BGGs and BCGs have very uniform masses, central ages and centralmetallicities. Examining the radial dependence of their stellar populations, wefind no significant velocity dispersion, age, or alpha-enhancement gradients.However, we find a wide range of metallicity gradients, suggesting a variety offormation mechanisms. The range of metallicity gradients observed is surprisinggiven the homogeneous environment these galaxies probe and their uniformcentral stellar populations. However, our results are inconsistent with anysingle model of galaxy formation and emphasize the need for more theoreticalunderstanding of both the origins of metallicity gradients and galaxy formationitself. We postulate two possible physical causes for the different formationmechanisms.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present the first result of the Ital-FLAMES survey of red giant branch(RGB) stars in omega Cen. Radial velocities with a precision of ~0.5 km/s arepresented for 650 members of omega Cen observed with FLAMES-Giraffe at the VeryLarge Telescope. We found that stars belonging to the metal -poor (RGB-MP),metal-intemediate (RGB-MInt) and metal-rich (RGB-a) sub -populations of OmegaCen are all compatible with having the same rotational pattern. Our resultsappear to contradict past findings by Norris et al., who could not detect anyrotational signature for metal -rich stars. The slightly higher precision ofthe present measurements and the much larger sample size, especially for themetal-richer stars, appear as the most likely explanation for this discrepancy.The result presented here weakens the body of evidence in favour of a mergerevent in the past history of omega Cen.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "This is the second of two papers reporting observations and analysis of theunusually bright (m_b=14.4), luminous (M_B=-25.5), nearby (z=0.192) narrow-linequasar PHL 1811. The first paper reported that PHL 1811 is intrinsically X-rayweak, and presented a spectral energy distribution (SED). Here we present HSTSTIS optical and UV spectra, and ground-based optical spectra. The optical andUV line emission is very unusual. There is no evidence for forbidden orsemiforbidden lines. The near-UV spectrum is dominated by very strong FeII andFeIII, and unusual low-ionization lines such as NaID and CaII H&K are observed.High-ionization lines are very weak; CIV has an equivalent width of 6.6A, afactor of ~5 smaller than measured from quasar composite spectra. An unusualfeature near 1200A can be deblended in terms of Ly\\alpha, NV, SiII, and CIII*using the blueshifted CIV profile as a template. Photoionization modeling showsthat the unusual line emission can be explained qualitatively by the unusuallysoft SED. Principally, a low gas temperature results in inefficient emission ofcollisionally excited lines, including the semiforbidden lines generally usedas density diagnostics. The emission resembles that of high-density gas; inboth cases this is a consequence of inefficient cooling. PHL 1811 is veryunusual, but we note that quasar surveys are generally biased against findingsimilar objects.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The science of complex networks is a new interdisciplinary branch of sciencewhich has arisen recently on the interface of physics, biology, social andcomputer sciences, and others. Its main goal is to discover general lawsgoverning the creation and growth as well as processes taking place onnetworks, like e.g. the Internet, transportation or neural networks. It turnedout that most real-world networks cannot be simply reduced to a compound ofsome individual components. Fortunately, the statistical mechanics, being oneof pillars of modern physics, provides us with a very powerful set of tools andmethods for describing and understanding these systems. In this thesis, wewould like to present a consistent approach to complex networks based onstatistical mechanics, with the central role played by the concept ofstatistical ensemble of networks. We show how to construct such a theory andpresent some practical problems where it can be applied. Among them, we payattention to the problem of finite-size corrections and the dynamics of asimple model of mass transport on networks.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We investigate the dimerization and fusion of C60 molecules to form variousC60 dimers when pushed against each other at several inter-molecular distances.We study the stability of this dimerized C60 molecule based on its bindingstrength provided by intramolecular interactions. Tersoff potential, which isconsidered to represent intramolecular interactions well, has been used tocalculate potential energy at these distances of separation and for allpossible orientations of the molecules. We observe that several minimum energyconfigurations exist at various distances between the C60 molecules. Ourcalculation shows that apart from the dumbbell structures, many interestingcomposite phases also result, such as fused, peanut and carbon nanotubes ofgeometry (5,5) and (10,0) of certain specific length.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Recently in \\cite{jss1}, the authors have given a method for calculation ofthe effective resistance (resistance distance) on distance-regular networks,where the calculation was based on stratification introduced in \\cite{js} andStieltjes transform of the spectral distribution (Stieltjes function)associated with the network. Also, in Ref. \\cite{jss1} it has been shown thatthe resistance distances between a node $\\alpha$ and all nodes $\\beta$belonging to the same stratum with respect to the $\\alpha$($R_{\\alpha\\beta^{(i)}}$, $\\beta$ belonging to the $i$-th stratum with respectto the $\\alpha$) are the same. In this work, an algorithm for recursivecalculation of the resistance distances in an arbitrary distance-regularresistor network is provided, where the derivation of the algorithm is based onthe Bose-Mesner algebra, stratification of the network, spectral techniques andChristoffel-Darboux identity. It is shown that the effective resistance on adistance-regular network is an strictly increasing function of the shortestpath distance defined on the network. In the other words, the two-pointresistance $R_{\\alpha\\beta^{(m+1)}}$ is strictly larger than$R_{\\alpha\\beta^{(m)}}$. The link between the resistance distance and randomwalks on distance-regular networks is discussed, where the average commute time(CT) and its square root (called Euclidean commute time (ECT)) as a distanceare related to the effective resistance. Finally, for some important examplesof finite distance- regular networks, the resistance distances are calculated.  {\\bf Keywords: resistance distance, association scheme, stratification,distance-regular networks, Christoffel-Darboux identity}  {\\bf PACs Index: 01.55.+b, 02.10.Yn}", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "This paper uncovers and explores the close relationship between Monte CarloOptimization of a parametrized integral (MCO), Parametric machine-Learning(PL), and `blackbox' or `oracle'-based optimization (BO). We make fourcontributions. First, we prove that MCO is mathematically identical to a broadclass of PL problems. This identity potentially provides a new applicationdomain for all broadly applicable PL techniques: MCO. Second, we introduceimmediate sampling, a new version of the Probability Collectives (PC) algorithmfor blackbox optimization. Immediate sampling transforms the original BOproblem into an MCO problem. Accordingly, by combining these first twocontributions, we can apply all PL techniques to BO. In our third contributionwe validate this way of improving BO by demonstrating that cross-validation andbagging improve immediate sampling. Finally, conventional MC and MCO proceduresignore the relationship between the sample point locations and the associatedvalues of the integrand; only the values of the integrand at those locationsare considered. We demonstrate that one can exploit the sample locationinformation using PL techniques, for example by forming a fit of the samplelocations to the associated values of the integrand. This provides anadditional way to apply PL techniques to improve MCO.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "High resolution molecular line observations of CS, HCO+, C18O and N2H+ wereobtained toward the starless globule FeSt 1-457 in order to investigate itskinematics and chemistry. The HCO+ and CS spectra show clear self-reversed andasymmetric profiles across the face of the globule. The sense of the observedasymmetry is indicative of the global presence of expansion motions in theouter layers of the globule. These motions appear to be subsonic andsignificantly below the escape velocity of the globule. Comparison of ourobservations with near-infrared extinction data indicate that the globule isgravitationally bound. Taken together these considerations lead us to suggestthat the observed expansion has its origin in an oscillatory motion of theouter layers of the globule which itself is likely in a quasi-stable state nearhydrostatic equilibrium. Analysis of the observed linewidths of CO and N2H+confirm that thermal pressure is the dominant component of the cloud's internalsupport. A simple calculation suggests that the dominant mode of pulsationwould be an l = 2 mode with a period of 0.3 Myr. Deformation of the globule dueto the large amplitude l = 2 oscillation may be responsible for thedouble-peaked structure of the core detected in high resolution extinctionmaps. Detailed comparison of the molecular-line observations and extinctiondata provides evidence for significant depletion of C18O and perhaps HCO+ whileN2H+ may be undepleted to a cloud depth of about 40 magnitudes of visualextinction.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We discuss the results from the combined IRAC and MIPS c2d Spitzer Legacyobservations of the Serpens star-forming region. In particular we present a setof criteria for isolating bona fide young stellar objects, YSO's, from theextensive background contamination by extra-galactic objects. We then discussthe properties of the resulting high confidence set of YSO's. We find 235 suchobjects in the 0.85 deg^2 field that was covered with both IRAC and MIPS. Anadditional set of 51 lower confidence YSO's outside this area is identifiedfrom the MIPS data combined with 2MASS photometry. We describe two sets ofresults, color-color diagrams to compare our observed source properties withthose of theoretical models for star/disk/envelope systems and our own modelingof the subset of our objects that appear to be star+disks. These objectsexhibit a very wide range of disk properties, from many that can be fit withactively accreting disks to some with both passive disks and even possiblydebris disks. We find that the luminosity function of YSO's in Serpens extendsdown to at least a few x .001 Lsun or lower for an assumed distance of 260 pc.The lower limit may be set by our inability to distinguish YSO's fromextra-galactic sources more than by the lack of YSO's at very low luminosities.A spatial clustering analysis shows that the nominally less-evolved YSO's aremore highly clustered than the later stages and that the backgroundextra-galactic population can be fit by the same two-point correlation functionas seen in other extra-galactic studies. We also present a table of matchesbetween several previous infrared and X-ray studies of the Serpens YSOpopulation and our Spitzer data set.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We investigate the problem of vortex trapping in cyclically coupledBose-Josephson junctions. Starting with $N$ independent BECs we couple thecondensates through Josephson links and allow the system to reach a stablecirculation by adding a dissipative term in our semiclassical equations ofmotion. The central question we address is what is the probability to trap avortex with winding number $m$. Our numerical simulations reveal that the finaldistribution of winding numbers is narrower than the initial distribution oftotal phases, indicating an increased probability for no-vortex configurations.Further, the nonlinearity of the problem manifests itself in the somewhatcounter-intuitive result that it is possible to obtain a non-zero circulationstarting with zero total phase around the loop. The final width of thedistribution of winding numbers for $N$ sites scales as $\\lambda N^{\\alpha}$,where $\\alpha=0.47\\pm 0.01$ and $\\lambda <0.67$ (value predicted for theinitial distribution) indicating a shrinking of the final distribution. Theactual value of $\\lambda$ is found to depend on the strength of dissipation.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "In the present paper a plastic-damage model for concrete is discussed. Basedon the fact that for isotropic materials the elastic trial stress and theprojected plastic stress states have the same eigenvec-tors, the loadingsurface is formulated in the principal stress space rather than using theinvariants of stress tensor. The model assumes that the directions oforthotropic damage coincide with principal directions of elastic predictorstress state (motivated by coaxial rotated crack model). Due to thisassumption, the load-ing surface and the closest point projection algorithm canstill be formulated in the principal directions. The evolution of the inelasticstrain is determined using minimization principle. Damage and plastic parts ofthe inelastic strain are separated using a scalar parameter, which is assumedto be stress dependent. The paper also discusses an effective numericalimplementation. The performance of the model is demonstrated on oneillustrative example.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We have measured resonance strengths and energies for dielectronicrecombination (DR) of Mg-like Fe XV forming Al-like Fe XIV via N=3 -> N' = 3core excitations in the electron-ion collision energy range 0-45 eV. Allmeasurements were carried out using the heavy-ion Test Storage Ring at the MaxPlanck Institute for Nuclear Physics in Heidelberg, Germany. We have alsocarried out new multiconfiguration Breit-Pauli (MCBP) calculations using theAUTOSTRUCTURE code. For electron-ion collision energies < 25 eV we find pooragreement between our experimental and theoretical resonance energies andstrengths. From 25 to 42 eV we find good agreement between the two forresonance energies. But in this energy range the theoretical resonancestrengths are ~ 31% larger than the experimental results. This is larger thanour estimated total experimental uncertainty in this energy range of +/- 26%(at a 90% confidence level). Above 42 eV the difference in the shape betweenthe calculated and measured 3s3p(^1P_1)nl DR series limit we attribute partlyto the nl dependence of the detection probabilities of high Rydberg states inthe experiment. We have used our measurements, supplemented by ourAUTOSTRUCTURE calculations, to produce a Maxwellian-averaged 3 -> 3 DR ratecoefficient for Fe XV forming Fe XIV. The resulting rate coefficient isestimated to be accurate to better than +/- 29% (at a 90% confidence level) fork_BT_e > 1 eV. At temperatures of k_BT_e ~ 2.5-15 eV, where Fe XV is predictedto form in photoionized plasmas, significant discrepancies are found betweenour experimentally-derived rate coefficient and previously publishedtheoretical results. Our new MCBP plasma rate coefficient is 19-28% smallerthan our experimental results over this temperature range.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Technological innovation has extensively been studied to make firmssustainable and more competitive. Within this context, the most importantrecent issue has been the dynamics of collaborative innovation among firms. Wetherefore investigated a patent network, especially focusing on its spatialcharacteristics. The results can be summarized as follows. (1) The degreedistribution in a patent network follows a power law. A firm can then beconnected to many firms via hubs connected to the firm. (2) The neighbors'average degree has a null correlation, but the clustering coefficient has anegative correlation. The latter means that there is a hierarchical structureand bridging different modules may shorten the paths between the nodes in them.(3) The distance of links not only indicates the regional accumulations offirms, but the importance of time it takes to travel, which plays a key role increating links. (4) The ratio of internal links in cities indicates that wehave to consider the existing links firms have to facilitate the creation ofnew links.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The spin-Hall effect in the two-dimensional electron gas (2DEG) generatessymmetric out-of-plane spin Sz accumulation about the current axis in theabsence of external magnetic field. Here we employ the real spaceLandauer-Keldysh formalism [B. K. Nikolic et al., Phys. Rev. Lett. 95, 046601(2005); Phys. Rev. B 73, 075303 (2006)] by considering a four-terminal setup toinvestigate the circumstances in which this symmetry is broken. For the absenceof Dresselhaus interaction, starting from the applied out-of-plane Bcorresponding to Zeeman splitting energy 0 - 0.5 times the Rashba hoppingenergy tR, the breaking process is clearly seen. The influence of the Rashbainteraction on the magnetization of the 2DEG is studied herein. For coexistedRashba tR and Dresselhaus tD spin-orbit couplings in the absence of B,interchanging tR and tD reverses the entire accumulation pattern.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We study in general the time-evolution of correlation functions in a extendedquantum system after the quench of a parameter in the hamiltonian. We show thatcorrelation functions in d dimensions can be extracted using methods ofboundary critical phenomena in d+1 dimensions. For d=1 this allows to use thepowerful tools of conformal field theory in the case of critical evolution.Several results are obtained in generic dimension in the gaussian (mean-field)approximation. These predictions are checked against the real-time evolution ofsome solvable models that allows also to understand which features are validbeyond the critical evolution.  All our findings may be explained in terms of a picture generally valid,whereby quasiparticles, entangled over regions of the order of the correlationlength in the initial state, then propagate with a finite speed through thesystem. Furthermore we show that the long-time results can be interpreted interms of a generalized Gibbs ensemble. We discuss some open questions andpossible future developments.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Instead of using local field equations - like the Dirac equation for spin-1/2and the Klein-Gordon equation for spin-0 particles - one could try to usenon-local field equations in order to describe scattering processes. The latterequations can be obtained by means of the relativistic energy together with thecorrespondence principle, resulting in equations with a square root operator.By coupling them to an electromagnetic field and expanding the square root (andtaking into account terms of quadratic order in the electromagnetic couplingconstant e), it is possible to calculate scattering matrix elements within theframework of quantum electrodynamics, e.g. like those for Compton scattering orfor the scattering of two identical particles. This will be done here for thescalar case. These results are then compared with the corresponding ones basedon the Klein-Gordon equation. A proposal of how to transfer these reflectionsto the spin-1/2 case is also presented.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We study the pseudospectrum of a class of non-selfadjoint differentialoperators. Our work consists in a detailed study of the microlocal properties,which rule the spectral stability or instability phenomena appearing undersmall perturbations for elliptic quadratic differential operators. The class ofelliptic quadratic differential operators stands for the class of operatorsdefined in the Weyl quantization by complex-valued elliptic quadratic symbols.We establish in this paper a simple necessary and sufficient condition on theWeyl symbol of these operators, which ensures the stability of their spectra.When this condition is violated, we prove that it occurs some strong spectralinstabilities for the high energies of these operators, in some regions whichcan be far away from their spectra. We give a precise geometrical descriptionof them, which explains the results obtained for these operators in somenumerical simulations giving the computation of false eigenvalues far fromtheir spectra by algorithms for eigenvalues computing.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "A cascade model is described based on multiplier distributions determinedfrom 3D direct numerical simulations (DNS) of turbulent particle laden flows,which include two-way coupling between the phases at global mass loadings equalto unity. The governing Eulerian equations are solved using pseudo-spectralmethods on up to 512**3 computional grid points. DNS results for particleconcentration and enstrophy at Taylor microscale Reynolds numbers in the range34 - 170 were used to directly determine multiplier distributions (PDFs) onspatial scales 3 times the Kolmogorov length scale. The width of the PDFs,which is a measure of intermittency, decreases with increasing mass loadingwithin the local region where the multipliers are measured. The functional formof this dependence is not sensitive to Reynolds numbers in the rangeconsidered. A partition correlation probability is included in the cascademodel to account for the observed spatial anticorrelation between particleconcentration and enstrophy. Joint probability distribution functions ofconcentration and enstrophy generated using the cascade model are shown to bein excellent agreement with those derived directly from our 3D simulations.Probabilities predicted by the cascade model are presented at Reynolds numberswell beyond what is achievable by direct simulation. These results clearlyindicate that particle mass loading significantly reduces the probabilities ofhigh particle concentration and enstrophy relative to those resulting fromunloaded runs. Particle mass density appears to reach a limit at around 100times the gas density. This approach has promise for significant computationalsavings in certain applications.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We study the expansion of the nearby Universe using a sample of Type Iasupernovae at redshifts below 0.08. These supernovae allow peculiar velocitiesto be measured at unprecedented precision. We have investigated in detail thepossibility of a varying Hubble constant with redshift and found no evidence ofa monopole term for the nearby Universe. A large scale streaming motion isfound at an amplitude of about $340^{63}_{-71}$ km/sec, aligned in thedirection of $(l_0, b_0) = (312^{\\rm o}.0^{13.5}_{-7.4}, 25^{\\rmo}.7^{8.0}_{-9.2})$, which is close to the direction of the center of Shapleysupercluster of galaxies. The large scale streaming motion is best fit by afunction involving a strong bipolar term. The streaming velocity field extendsfrom the lowest redshift ($\\sim 0.007$) to beyond 0.025 and likely out to evenhigher redshifts. The velocity field at redshift below 0.01 can be equally welldescribed by a dipole field or by the same bipolar streaming velocity fieldthat reaches out to beyond $z \\sim 0.025$. We are also able to deduce a robustestimate of the random velocity component of the peculiar velocity field.Within the volume of redshift below 0.01 (weighted average redshift of $\\sim$0.067), this thermal component is found to be about 270 km/sec. Aftercorrecting this smooth streaming motion, we are able to significantly improvethe Hubble expansion fits of these supernovae. The CMAGIC method gives adramatic decrease of $\\chi^2$ from 90 to 63 for 69 degrees of freedom, andyields a residual scatter of only 0.12 magnitude; the maximum light methodgives also a moderate improvement.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "For a smooth projective curve, the cycles of e-secant k-planes are among themost studied objects in classical enumerative geometry and there are well-knownformulas due to Castelnuovo, Cayley and MacDonald concerning them. Despitevarious attempts, surprisingly little is known about the enumerative validityof such formulas. The aim of this paper is to completely clarify this problemin the case of the generic curve C of given genus. Using degenerationtechniques and a few facts about the birational geometry of moduli spaces ofstable pointed curves we determine precisely under which conditions the cycleof e-secant k-planes in non-empty and we compute its dimension. We alsoprecisely determine the dimension of the variety of linear series on C carryinge-secant k-planes. In a different direction, in the last part of the paper westudy the distribution of ramification points of the powers of a line bundle onC having prescribed ramification at a given point.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Spatial associations have been found between interstellar neutral hydrogen(HI) emission morphology and small-scale structure observed by the WilkinsonMicrowave Anisotropy Probe (WMAP) in an area bounded by l = 60 & 180 deg, b =30 & 70 deg, which was the primary target for this study. This area is markedby the presence of highly disturbed local HI and a preponderance ofintermediate- and high-velocity gas. The HI distribution toward the brightestpeaks in the WMAP Internal Linear Combination (ILC) map for this area isexamined and by comparing with a second area on the sky it is demonstrated thatthe associations do not appear to be the result of chance coincidence. Closeexamination of several of the associations reveals important new properties ofdiffuse interstellar neutral hydrogen structure. In the case of high-velocitycloud MI, the HI and WMAP ILC morphologies are similar and an excess of softX-ray emission and H-alpha emission have been reported for this feature. It issuggested that the small angular-scale, high frequency continuum emissionobserved by WMAP may be produced at the surfaces of HI features interacting oneanother, or at the interface between moving HI structures and regions ofenhanced plasma density in the surrounding interstellar medium. It is possiblethat dust grains play a role in producing the emission. However, the primarypurpose of this report is to draw attention to these apparent associationswithout offering an unambiguous explanation as to the relevant emissionmechanism(s).", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We report on transcritical bifurcations of periodic orbits in non-integrabletwo-dimensional Hamiltonian systems. We discuss their existence criteria andsome of their properties using a recent mathematical description oftranscritical bifurcations in families of symplectic maps. We then presentnumerical examples of transcritical bifurcations in a class of generalizedH\\'enon-Heiles Hamiltonians and illustrate their stabilities and unfoldingsunder various perturbations of the Hamiltonians. We demonstrate that forHamiltonians containing straight-line librating orbits, the transcriticalbifurcation of these orbits is the typical case which occurs also in theabsence of any discrete symmetries, while their isochronous pitchforkbifurcation is an exception. We determine the normal forms of both types ofbifurcations and derive the uniform approximation required to includetranscritically bifurcating orbits in the semiclassical trace formula for thedensity of states of the quantum Hamiltonian. We compute the coarse-graineddensity of states in a specific example both semiclassically and quantummechanically and find excellent agreement of the results.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Past work has shown that ions can pass through a membrane more readily in onedirection than the other. We demonstrate here in a model and an experiment thatfor a mixture of small and large particles such asymmetric diffusion can arisesolely from an asymmetry in the geometry of the pores of the membrane. Ourdeterministic simulation considers a two-dimensional gas of elastic disks oftwo sizes diffusing through a membrane, and our laboratory experiment examinesthe diffusion of glass beads of two sizes through a metal membrane. In bothexperiment and simulation, the membrane is permeable only to the smallerparticles, and the asymmetric pores lead to an asymmetry in the diffusion ratesof these particles. The presence of even a small percentage of large particlescan clog a membrane, preventing passage of the small particles in one directionwhile permitting free flow of the small particles in the other direction. Thepurely geometric kinetic constraints may play a role in common biologicalcontexts such as membrane ion channels.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We evaluate the possibility of observable effects arising from collisionsbetween vacuum bubbles in a universe undergoing false-vacuum eternal inflation.Contrary to conventional wisdom, we find that under certain assumptions mostpositions inside a bubble should have access to a large number of collisionevents. We calculate the expected number and angular size distribution of suchcollisions on an observer's \"sky,\" finding that for typical observers thedistribution is anisotropic and includes many bubbles, each of which willaffect the majority of the observer's sky. After a qualitative discussion ofthe physics involved in collisions between arbitrary bubbles, we evaluate theimplications of our results, and outline possible detectable effects. In anoptimistic sense, then, the present paper constitutes a first step in anassessment of the possible effects of other bubble universes on the cosmicmicrowave background and other observables.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present the first detailed study of the properties (temperatures,gravities, and masses) of the NGC 6791 white dwarf population. This uniquestellar system is both one of the oldest (8 Gyr) and most metal-rich ([Fe/H] ~0.4) open clusters in our Galaxy, and has a color-magnitude diagram (CMD) thatexhibits both a red giant clump and a much hotter extreme horizontal branch.Fitting the Balmer lines of the white dwarfs in the cluster, using Keck/LRISspectra, suggests that most of these stars are undermassive, <M> = 0.43 +/-0.06 Msun, and therefore could not have formed from canonical stellar evolutioninvolving the helium flash at the tip of the red giant branch. We show that atleast 40% of NGC 6791's evolved stars must have lost enough mass on the redgiant branch to avoid the flash, and therefore did not convert helium intocarbon-oxygen in their core. Such increased mass loss in the evolution of theprogenitors of these stars is consistent with the presence of the extremehorizontal branch in the CMD. This unique stellar evolutionary channel alsonaturally explains the recent finding of a very young age (2.4 Gyr) for NGC6791 from white dwarf cooling theory; helium core white dwarfs in this clusterwill cool ~3 times slower than carbon-oxygen core stars and therefore thecorrected white dwarf cooling age is in fact ~7 Gyr, consistent with the wellmeasured main-sequence turnoff age. These results provide direct empiricalevidence that mass loss is much more efficient in high metallicity environmentsand therefore may be critical in interpreting the ultraviolet upturn inelliptical galaxies.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The physical characteristics of the Lyman-alpha forest cloud systems arecombined with observations on the baryonic mass density of the Universe andconstraints from primordial nucleosynthesis to set boundary conditions on theIntergalactic Medium (IGM) at the epoch of z=2.5. The Universe is considered aclosed system and allowed to expand adiabatically from the epoch when QSOsfirst ionized the IGM (5 <= z_on <= 20). The average kinetic energy of a gas iscalculated in the region where the gas transitions from relativistic tonon-relativistic behavior. All of the above measurements are then used todetermine the thermal history of the IGM in the redshift range 2.5 <= z <=z_on. The hot IGM is assumed to inverse Compton scatter photons from the CosmicMicrowave Background (CMBR) and consequently distort the CMBR as seen at thepresent epoch. The temperature of the IGM at z=2.5 and the epoch z_on areadjusted, within the constraints defined above, to give the best overallagreement with published data on the temperature of the IGM. We find that themodel of the IGM proposed here does not grossly distort the CMBR, and in factagrees quite closely with the preliminary results from the Cosmic BackgroundExplorer (COBE) satellite. However, our model of the IGM cannot explain theobserved cosmic x ray background.  This paper was originally written in 1990. It was never submitted forpublication.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Arguments showing that exchange-only optimized effective potential (xOEP)methods, with finite basis sets, cannot in general yield the Hartree-Fock (HF)ground state energy, but a higher one, are given. While the orbital products ofa complete basis are linearly dependent, the HF ground state energy can only beobtained via a basis set xOEP scheme in the special case that all products ofoccupied and unoccupied orbitals emerging from the employed orbital basis setare linearly independent from each other. In this case, however, exchangepotentials leading to the HF ground state energy exhibit unphysicaloscillations and do not represent a Kohn-Sham (KS) exchange potential. Thesefindings solve the seemingly paradoxical results of Staroverov, Scuseria andDavidson that certain finite basis set xOEP calculations lead to the HF groundstate energy despite the fact that within a real space (or complete basis)representation the xOEP ground state energy is always higher than the HFenergy. Moreover, whether or not the occupied and unoccupied orbital productsare linearly independent, it is shown that basis set xOEP methods onlyrepresent exact exchange-only (EXX) KS methods, i.e., proper density-functionalmethods, if the orbital basis set and the auxiliary basis set representing theexchange potential are balanced to each other, i.e., if the orbital basis iscomprehensive enough for a given auxiliary basis. Otherwise xOEP methods do notrepresent EXX KS methods and yield unphysical exchange potentials.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We construct a family of equations of state within a quasiparticle model byrelating pressure, energy density, baryon density and susceptibilities adjustedto first-principles lattice QCD calculations. The relation between pressure andenergy density from lattice QCD is surprisingly insensitive to details of thesimulations. Effects from different lattice actions, quark masses and latticespacings used in the simulations show up mostly in the quark-hadron phasetransition region which we bridge over by a set of interpolations to a hadronresonance gas equation of state. Within our optimized quasiparticle model wethen examine the equation of state along isentropic expansion trajectories atsmall net baryon densities, as relevant for experiments and hydrodynamicsimulations at RHIC and LHC energies. We illustrate its impact on azimuthalflow anisotropies and transverse momentum spectra of various hadron species.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "This paper focuses on supergravity duals of BPS states in N=4 superYang-Mills. In order to describe these duals, we begin with a sequence ofbreathing mode reductions of IIB supergravity: first on S^3, then S^3 x S^1,and finally on S^3 x S^1 x CP^1. We then follow with a complete supersymmetryanalysis, yielding 1/8, 1/4 and 1/2 BPS configurations, respectively (where inthe last step we take the Hopf fibration of S^3). The 1/8 BPS geometries, whichhave an S^3 isometry and are time-fibered over a six-dimensional base, aredetermined by solving a non-linear equation for the Kahler metric on the base.Similarly, the 1/4 BPS configurations have an S^3 x S^1 isometry and afour-dimensional base, whose Kahler metric obeys another non-linear,Monge-Ampere type equation.  Despite the non-linearity of the problem, we develop a universal bubbling AdSdescription of these geometries by focusing on the boundary conditions whichensure their regularity. In the 1/8 BPS case, we find that the S^3 cycleshrinks to zero size on a five-dimensional locus inside the six-dimensionalbase. Enforcing regularity of the full solution requires that the interior of asmooth, generally disconnected five-dimensional surface be removed from thebase. The AdS_5 x S^5 ground state corresponds to excising the interior of anS^5, while the 1/8 BPS excitations correspond to deformations (includingtopology change) of the S^5 and/or the excision of additional droplets from thebase. In the case of 1/4 BPS configurations, by enforcing regularityconditions, we identify three-dimensional surfaces inside the four-dimensionalbase which separate the regions where the S^3 shrinks to zero size from thosewhere the S^1 shrinks.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present new multicolor photo-polarimetry of stars behind the SouthernCoalsack. Analyzed together with multiband polarization data from theliterature, probing the Chamaeleon I, Musca, rho Opiuchus, R CrA and Taurusclouds, we show that the wavelength of maximum polarization (lambda_max) islinearly correlated with the radiation environment of the grains. UsingFar-Infrared emission data, we show that the large scatter seen in previousstudies of lambda_max as a function of A_V is primarily due to line of sighteffects causing some A_V measurements to not be a good tracer of the extinction(radiation field strength) seen by the grains being probed. The derived slopesin lambda_max vs. A_V, for the individual clouds, are consistent with a commonvalue, while the zero intercepts scale with the average values of the ratios oftotal-to-selective extinction (R_V) for the individual clouds. Within eachcloud we do not find direct correlations between lambda_max and R_V. Thepositive slope in consistent with recent developments in theory and indicatingalignment driven by the radiation field. The present data cannot conclusivelydifferentiate between direct radiative torques and alignment driven by H_2formation. However, the small values of lambda_max(A_V=0), seen in severalclouds, suggest a role for the latter, at least at the cloud surfaces. Thescatter in the lambda_max vs. A_V relation is found to be associated with thecharacteristics of the embedded Young Stellar Objects (YSO) in the clouds. Wepropose that this is partially due to locally increased plasma damping of thegrain rotation caused by X-rays from the YSOs.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "In this paper we present a new mathematical model for the density regionswhere a specific spectral line and its SACs/DACs are created in the Oe and Bestellar atmospheres. In the calculations of final spectral line function weconsider that the main reasons of the line broadening are the rotation of thedensity regions creating the spectral line and its DACs/SACs, as well as therandom motions of the ions. This line function is able to reproduce thespectral feature and it enables us to calculate some important physicalparameters, such as the rotational, the radial and the random velocities, theFull Width at Half Maximum, the Gaussian deviation, the optical depth, thecolumn density and the absorbed or emitted energy. Additionally, we cancalculate the percentage of the contribution of the rotational velocity and theions' random motions of the DACs/SACs regions to the line broadening. Finally,we present two tests and three short applications of the proposed model.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We investigate the Gross-Pitaevskii equation for a classically chaoticsystem, which describes an atomic Bose-Einstein condensate confined in anoptical lattice and driven by a spatiotemporal periodic laser field. It isdemonstrated that the exact Floquet states appear when the externaltime-dependent potential is balanced by the nonlinear mean-field interaction.The balance region of parameters is divided into a phase-continuing region anda phase-jumping one. In the latter region, the Floquet states arespatiotemporal vortices of nontrivial phase structures and zero-density cores.Due to the velocity singularities of vortex cores and the blowing-up ofperturbed solutions, the spatiotemporal vortices are unstable periodic statesembedded in chaos. The stability and instability of these Floquet states arenumerically explored by the time evolution of fidelity between the exact andnumerical solutions. It is numerically illustrated that the stable Floquetstates could be prepared from the uniformly initial states by slow growth ofthe external potential.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We utilize a recent formulation of a spherically symmetric spacetime endowedwith a general decomposition of the energy momentum tensor [Phys. Rev. D, 75,024031 (2007)] to derive equations governing spherically symmetricdistributions of electromagnetic matter. We show the system reduces to theReissner-Nordstrom spacetime in general, spherically symmetric coordinates inthe vacuum limit. Furthermore, we show reduction to the charged Vaidyaspacetime in non-null coordinates when certain equations of states are chosen.A model of gravitational collapse is discussed whereby a charged fluid resideswithin a boundary of finite radial extent on the initial hypersurface, and isallowed to radiate charged particles. Our formalism allows for the discussionof all regions in this model without the need for complicated matching schemesat the interfaces between successive regions. As further examples we considerthe collapse of a thin shell of charged matter onto a Reissner-Nordstrom blackhole. Finally, we reduce the entire system of equations to the static case suchthat we have the equations for hydrostatic equilibrium of a charged fluid.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The 105-ms X-ray pulsar J1852+0040 is the central compact object (CCO) in SNRKes 79. We report a sensitive upper limit on its radio flux density of 12 uJyat 2 GHz using the NRAO GBT. Timing using XMM and Chandra over a 2.4 yr spanreveals no significant change in its spin period. The 2 sigma upper limit onthe period derivative leads, in the dipole spin-down formalism, to an energyloss rate E-dot < 7e33 ergs/s, surface magnetic field strength B_p < 1.5e11 G,and characteristic age tau_c = P/2P-dot > 8 Myr. This tau_c exceeds the age ofthe SNR by 3 orders of magnitude, implying that the pulsar was born spinning atits current period. However, the X-ray luminosity of PSR J1852+0040, L(bol) ~3e33(d/7.1 kpc)^2 ergs/s is a large fraction of E-dot, which challenges therotation-powered assumption. Instead, its high blackbody temperature,0.46+/-0.04 keV, small blackbody radius ~ 0.8 km, and large pulsed fraction, ~80%, may be evidence of accretion onto a polar cap, possibly from a fallbackdisk made of supernova debris. If B_p < 1e10 G, an accretion disk can penetratethe light cylinder and interact with the magnetosphere while resulting torqueson the neutron star remain within the observed limits. A weak B-field is alsoinferred in another CCO, the 424-ms pulsar 1E 1207.4-5209, from its steady spinand soft X-ray absorption lines. We propose this origin of radio-quiet CCOs:the B-field, derived from a turbulent dynamo, is weaker if the NS is formedspinning slowly, which enables it to accrete SN debris. Accretion excludesneutron stars born with both B_p < 1e11 G and P > 0.1 s from radio pulsarsurveys, where B_p < 1e11 G is not encountered except among very old (tau_c >40 Myr) or recycled pulsars. Finally, such a CCO, if born in SN 1987A, couldexplain the non-detection of a pulsar there.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Order(N) Tight-Binding Molecular Dynamics (TBMD) simulations are performed toinvestigate the thermal stability of (10,10) metallic Single-Walled CarbonNanotubes (SWCNT). Periodic boundary conditions (PBC) are applied in axialdirection. Velocity Verlet algorithm along with the canonical ensemblemolecular dynamics (NVT) is used to simulate the tubes at the targetedtemperatures. The effects of slow and rapid temperature increases on thephysical characteristics, structural stability and the energetics of the tubeare investigated and compared. Simulations are carried out starting from roomtemperature and the temperature is raised in steps of 300K. Stability of thesimulated metallic SWCNT is examined at each step before it is heated to highertemperatures. First indication of structural deformation is observed at 600K.For higher heat treatments the deformations are more pronounced and the bondbreaking temperature is reached around 2500K. Gradual (slow) heating andthermal equilibrium (fast heating) methods give the value of radial thermalexpansion coefficient in the temperature range between 300K-600K as0.31x10^{-5}(1/K) and 0.089x10^{-5}(1/K), respectively. After 600K, bothmethods give the same value of 0.089x10^{-5}(1/K). The ratio of the totalenergy per atom with respect to temperature is found to be 3x10^{-4} eV/K.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "(Abridged) Using cosmological hydrodynamic simulations in combination withanalytic modeling, we show that the galaxy stellar mass-metallicity relation(MZR) provides strong constraints on galactic outflows across cosmic time. Wecompare three outflow models: No outflows, a \"constant wind\" (cw) model thatemulates the popular Dekel & Silk (1986) scenario, and a ``momentum-drivenwind\" (vzw) model. We find that only the vzw scaling reproduces the observedz~2 MZR's slope, amplitude, and scatter. Comparing our fully three-dimensionalsimulations with a simple one-zone chemical evolution model, we find that theMZR can be understood in terms of three parameters: (1) The equilibriummetallicity Z_eq=y*SFR/ACC (where y=true yield), reflecting the enrichmentbalance between star formation rate SFR and gas accretion rate ACC; (2) thedilution time t_d=M_g/ACC, representing the timescale for a galaxy to return toZ_eq after a metallicity-perturbing interaction; and (3) the blowout massM_blowout, which is the galaxy stellar mass above which winds can escape itshalo. When outflows with mass loading factor MLF are present, galaxies belowM_blowout obey Z_eq = y/(1+MLF), while above M_blowout, Z_eq->y. Our cw modelhas M_blowout ~ 10^10 M_sun, which yields a sharp upturn in the MZR above thisscale and a flat MZR with large scatter below it, in strong disagreement withobservations. Our vzw model reproduces the observed Z_g \\propto M_*^0.3 becauseZ_eq \\propto MLF^-1 \\propto M_*^1/3 when MLF >> 1 (i.e. at low masses). Theflattening of the MZR at M_* > 10^10.5 M_sun observed by Tremonti et al. (2004)reflects the mass scale where MLF~1, rather than a characteristic wind speed.The tight observed MZR scatter is ensured when t_d<1 dynamical time, which isonly satisified at all masses and epochs in our momentum-driven wind model.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present broadband NIR spectra of A0620-00 obtained with SpeX on the IRTF.The spectrum is characterized by a blue continuum on which are superimposedbroad emission lines of HI and HeII and a host of narrower absorption lines ofneutral metals and molecules. Spectral type standard star spectra scaled to thedereddened spectrum of A0620-00 in K exceed the A0620-00 spectrum in J and Hfor all stars of spectral type K7V or earlier, demonstrating that the donorstar, unless later than K7V, cannot be the sole NIR flux source in A0620-00. Inaddition, the atomic absorption lines in the K3V spectrum are too weak withrespect to those of A0620-00 even at 100% donor star contribution, restrictingthe spectral type of the donor star in A0620-00 to later than K3V. Comparisonof the A0620-00 spectrum to scaled K star spectra indicates that the COabsorption features are significantly weaker in A0620-00 than in field dwarfstars. Fits of scaled model spectra of a Roche lobe-filling donor star to thespectrum of A0620-00 show that the best match to the CO absorption lines isobtained when the C abundance is reduced to [C/H] = -1.5. The donor starcontribution in the H waveband is determined to be 82+-2%. Combined withprevious published results from Froning & Robinson (2001) and Marsh et al.(1994), this gives a precise mass for the black hole in A0620-00 of M_BH =9.7+-0.6 M_solar.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "There exist methods for determining effective conservative interactions incoarse grained particle based mesoscopic simulations. The resulting models canbe used to capture thermal equilibrium behavior, but in the model system westudy do not correctly represent transport properties. In this article wesuggest the use of force covariance to determine the full functional form ofdissipative and stochastic interactions. We show that a combination of theradial distribution function and a force covariance function can be used todetermine all interactions in dissipative particle dynamics. Furthermore we usethe method to test if the effective interactions in dissipative particledynamics (DPD) can be adjusted to produce a force covariance consistent with aprojection of a microscopic Lennard-Jones simulation. The results indicate thatthe DPD ansatz may not be consistent with the underlying microscopic dynamics.We discuss how this result relates to theoretical studies reported in theliterature.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "In the work, the new method for the design of the wavelength divisionmultiplexer on the basis of 2D photonic crystal integrated circuit for theultra-short pulses channel separation is proposed and investigated. The methodis based on the analysis of full photonic bandgap maps that allows defining theultra-short pulse demultiplexer parameters selection. For the methodapprobation, there was synthesized the device in which the wideband filters areused for the channel separation. As it was expected, the device effectivelyseparates 50 fs pulse channels with 1.31 and 1.55 microns wavelengths. Theobtained spectral characteristics and pulse pattern responses validate theefficiency of the proposed method and the applicability of such devices to theintegrated photonic information processing circuits.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We study the evolution of a neutral $K$ meson prepared as an incoherent equalmixture of $K^0$ and $\\bar{K^0}$. Denoting the density matrix by $\\rho(t) ={1/2} N(t) [\\1 + \\vec{\\zeta}(t) \\cdot \\vec{\\sigma} ] $, the norm of the state$N(t)$ is found to decrease monotonically from one to zero, while the magnitudeof the Stokes vector $|\\vec{\\zeta}(t)|$ increases monotonically from zero toone. This property qualifies these observables as arrows of time. Requiringmonotonic behaviour of $N(t)$ for arbitrary values of $\\gamma_L, \\gamma_S$ and$\\Delta m$ yields a bound on the CP-violating overlap $\\delta =\\braket{K_L}{K_S}$, which is similar to, but weaker than, the known unitaritybound. A similar requirement on $|\\vec{\\zeta}(t)|$ yields a new bound,$\\delta^2 < {1/2} (\\frac{\\Delta \\gamma}{\\Delta m}) \\sinh (\\frac{3\\pi}{4}\\frac{\\Delta \\gamma}{\\Delta m})$ which is particularly effective in limitingthe CP-violating overlap in the $B^0$-$\\bar{B^0}$ system. We obtain the Stokesparameter $\\zeta_3(t)$ which shows how the average strangeness of the beamevolves from zero to $\\delta$. The evolution of the Stokes vector from$|\\vec{\\zeta}| = 0$ to $|\\vec{\\zeta}| = 1$ has a resemblance to an orderparameter of a system undergoing spontaneous symmetry breaking.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We consider maximum solution $g(t)$, $t\\in [0, +\\infty)$, to the normalizedRicci flow. Among other things, we prove that, if $(M, \\omega) $ is a smoothcompact symplectic 4-manifold such that $b_2^+(M)>1$ and let$g(t),t\\in[0,\\infty)$, be a solution to (1.3) on $M$ whose Ricci curvaturesatisfies that $|\\text{Ric}(g(t))|\\leq 3$ and additionally $\\chi(M)=3 \\tau(M)>0$, then there exists an $m\\in \\mathbb{N}$, and a sequence of points$\\{x_{j,k}\\in M\\}$, $j=1, ..., m$, satisfying that, by passing to asubsequence, $$(M, g(t_{k}+t), x_{1,k},..., x_{m,k})\\stackrel{d_{GH}}\\longrightarrow (\\coprod_{j=1}^m N_j, g_{\\infty},x_{1,\\infty}, ...,, x_{m,\\infty}),$$ $t\\in [0, \\infty)$, in the $m$-pointedGromov-Hausdorff sense for any sequence $t_{k}\\longrightarrow \\infty$, where$(N_{j}, g_{\\infty})$, $j=1,..., m$, are complete complex hyperbolic orbifoldsof complex dimension 2 with at most finitely many isolated orbifold points.Moreover, the convergence is $C^{\\infty}$ in the non-singular part of$\\coprod_1^m N_{j}$ and$\\text{Vol}_{g_{0}}(M)=\\sum_{j=1}^{m}\\text{Vol}_{g_{\\infty}}(N_{j})$, where$\\chi(M)$ (resp. $\\tau(M)$) is the Euler characteristic (resp. signature) of$M$.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We study five-dimensional black holes obtained by compactifying M theory onCalabi-Yau threefolds. Recent progress in solving topological string theory oncompact, one-parameter models allows us to test numerically various conjecturesabout these black holes. We give convincing evidence that a microscopicdescription based on Gopakumar-Vafa invariants accounts correctly for theirmacroscopic entropy, and we check that highly nontrivial cancellations -whichseem necessary to resolve the so-called entropy enigma in the OSV conjecture-do in fact occur. We also study analytically small 5d black holes obtained bywrapping M2 branes in the fiber of K3 fibrations. By using heterotic/type IIduality we obtain exact formulae for the microscopic degeneracies in variousgeometries, and we compute their asymptotic expansion for large charges.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We study the effects produced by D-brane instantons on the holomorphicquantities of a D-brane gauge theory at an orbifold singularity. These effectsare not limited to reproducing the well known contributions of the gauge theoryinstantons but also generate extra terms in the superpotential or theprepotential. On these brane instantons there are some neutral fermioniczero-modes in addition to the ones expected from broken supertranslations. Theyare crucial in correctly reproducing effects which are dual to gauge theoryinstantons, but they may make some other interesting contributions vanish. Weanalyze how orientifold projections can remove these zero-modes and thus allowfor new superpotential terms. These terms contribute to the dynamics of theeffective gauge theory, for instance in the stabilization of runawaydirections.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present observations of pure rotational molecular hydrogen emission fromthe Herbig Ae star, AB Aurigae. Our observations were made using the TexasEchelon Cross Echelle Spectrograph (TEXES) at the NASA Infrared TelescopeFacility and the Gemini North Observatory. We searched for H2 emission in theS(1), S(2), and S(4) lines at high spectral resolution and detected all three.By fitting a simple model for the emission in the three transitions, we deriveT = 670 +/- 40 K and M = 0.52 +/- 0.15 earth masses for the emitting gas. Basedon the 8.5 km/s FWHM of the S(2) line, assuming the emission comes from thecircumstellar disk, and with an inclination estimate of the AB Aur system takenfrom the literature, we place the location for the emission near 18 AU.Comparison of our derived temperature to a disk structure model suggests thatUV and X-ray heating are important in heating the disk atmosphere.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "BACKGROUND: An important question is whether evolution favors properties suchas mutational robustness or evolvability that do not directly benefit anyindividual, but can influence the course of future evolution. Functionallysimilar proteins can differ substantially in their robustness to mutations andcapacity to evolve new functions, but it has remained unclear whether any ofthese differences might be due to evolutionary selection for these properties.  RESULTS: Here we use laboratory experiments to demonstrate that evolutionfavors protein mutational robustness if the evolving population is sufficientlylarge. We neutrally evolve cytochrome P450 proteins under identical selectionpressures and mutation rates in populations of different sizes, and show thatproteins from the larger and thus more polymorphic population tend towardshigher mutational robustness. Proteins from the larger population also evolvegreater stability, a biophysical property that is known to enhance bothmutational robustness and evolvability. The excess mutational robustness andstability is well described by existing mathematical theories, and can bequantitatively related to the way that the proteins occupy their neutralnetwork.  CONCLUSIONS: Our work is the first experimental demonstration of the generaltendency of evolution to favor mutational robustness and protein stability inhighly polymorphic populations. We suggest that this phenomenon may contributeto the mutational robustness and evolvability of viruses and bacteria thatexist in large populations.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We report a computational first-principles study of positron trapping atvacancy defects in metals and semiconductors. The main emphasis is on theenergetics of the trapping process including the interplay between the positronstate and the defect's ionic structure and on the ensuing annihilationcharacteristics of the trapped state. For vacancies in covalent semiconductorsthe ion relaxation is a crucial part of the positron trapping process enablingthe localization of the positron state. However, positron trapping does notstrongly affect the characteristic features of the electronic structure, e.g.,the ionization levels change only moderately. Also in the case of metalvacancies the positron-induced ion relaxation has a noticeable effect on thecalculated positron lifetime and momentum distribution of annihilatingelectron-positron pairs.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Berry phases and the quantum-information theoretic notion of fidelity havebeen recently used to analyze quantum phase transitions from a geometricalperspective. In this paper we unify these two approaches showing that theunderlying mechanism is the critical singular behavior of a complex tensor overthe Hamiltonian parameter space. This is achieved by performing a scalinganalysis of this quantum geometric tensor in the vicinity of the criticalpoints. In this way most of the previous results are understood on generalgrounds and new ones are found. We show that criticality is not a sufficientcondition to ensure superextensive divergence of the geometric tensor, andstate the conditions under which this is possible. The validity of thisanalysis is further checked by exact diagonalization of the spin-1/2 XXZHeisenberg chain.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The mass loss properties of carbon AGB stars are not very well constrained atpresent. A variety of empirical or theoretical formulae with differentparameterisations are available in the literature and the agreement betweenthem is anything but good. These simple mass loss prescriptions are nonthelessused in many models of stellar evolution without much consideration of theirapplicability in various cases. We present here an on-going project aiming at abetter description of the mass loss, that could be used to improve stellarevolution models -- especially the evolution during the TP-AGB phase. As afirst step, we have considered the mass loss evolution during a He-shell flash.Using stellar parameters sampled from a stellar evolutionary track, we havecomputed the time evolution of the atmospheric layers and wind accelerationregion during a flash event with detailed frequency-dependentradiation-hydrodynamical models including dust formation. Based on theseresults, we have also simulated the subsequent long-term dynamical evolution ofthe circumstellar envelope (CSE), including the formation of a detached shell.We find that existing simple mass loss prescriptions imply different mass lossevolutions compared with our model. The second step of the project deals withthe dependence of mass loss on the basic stellar parameters. At the moment weare computing a large grid of wind models for C-rich AGB stars. Preliminaryresults show that simple parameterisations are difficult to obtain in certainregions of the parameter space considered, due to strong non-linearities in thewind mechanism.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "A number of recently discovered protein structures incorporate a ratherunexpected structural feature: a knot in the polypeptide backbone. These knotsare extremely rare, but their occurrence is likely connected to proteinfunction in as yet unexplored fashion. Our analysis of the complete ProteinData Bank reveals several new knots which, along with previously discoveredones, can shed light on such connections. In particular, we identify the mostcomplex knot discovered to date in human ubiquitin hydrolase, and suggest thatits entangled topology protects it against unfolding and degradation by theproteasome. Knots in proteins are typically preserved across species andsometimes even across kingdoms. However, we also identify a knot which onlyappears in some transcarbamylases while being absent in homologous proteins ofsimilar structure. The emergence of the knot is accompanied by a shift in theenzymatic function of the protein. We suggest that the simple insertion of ashort DNA fragment into the gene may suffice to turn an unknotted into aknotted structure in this protein.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Electron-electron interactions play a major role in determining thelow-temperature rate of phase loss of electrons in mesoscopic systems. Thestudy of the dephasing rate is expected to contribute to the understanding ofthe many-body nature of such systems. Closed quantum dots are of specialinterest in this respect, due to theoretical predictions suggesting a possibletransition temperature below which the dephasing rate vanishes. This predictionhas attracted much attention, since closed quantum dots are prime candidatesfor storage units in quantum computers, and thus their phase coherenceproperties are of great importance. However, an effective method for measuringthe dephasing rate within a closed quantum dot is still lacking. Here we studytwo-level systems and show that the Fano factor has a sharp peak as a functionof the chemical potential, the location of which can be simply related to thedephasing rate. We thus suggest to use the properties of the Fano factor peakin the super-Poissonian regime as a probe for the dephasing rate.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "In braneworld cosmology the expanding Universe is realized as a brane movingthrough a warped higher-dimensional spacetime. Like a moving mirror causes thecreation of photons out of vacuum fluctuations, a moving brane leads tograviton production. We show that, very generically, Kaluza-Klein (KK)particles scale like stiff matter with the expansion of the Universe and cantherefore not represent the dark matter in a warped braneworld. We presentresults for the production of massless and KK gravitons for bouncing branes infive-dimensional anti de Sitter space. We find that for a realistic bounce theback reaction from the generated gravitons will be most likely relevant. Thisletter summarizes the main results and conclusions from numerical simulationswhich are presented in detail in a long paper [M.Ruser and R. Durrer, Phys.Rev. D 76, 104014 (2007), arXiv:0704.0790]", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Employing Big Bear Solar Observatory (BBSO) deep magnetograms and H${\\alpha}$images in a quiet region and a coronal hole, observed on September 14 and 16,2004, respectively, we have explored the magnetic flux emergence, disappearanceand distribution in the two regions. The following results are obtained: (1)The evolution of magnetic flux in the quiet region is much faster than that inthe coronal hole, as the flux appeared in the form of ephemeral regions in thequiet region is 4.3 times as large as that in the coronal hole, and the fluxdisappeared in the form of flux cancellation, 2.9 times as fast as in thecoronal hole. (2) More magnetic elements with opposite polarities in the quietregion are connected by arch filaments, estimating from magnetograms andH${\\alpha}$ images. (3) We measured the magnetic flux of about 1000 magneticelements in each observing region. The flux distribution of network andintranetwork (IN) elements is similar in both polarities in the quiet region.For network fields in the coronal hole, the number of negative elements is muchmore than that of positive elements. However for the IN fields, the number ofpositive elements is much more than that of negative elements. (4) In thecoronal hole, the fraction of negative flux change obviously with differentthreshold flux density. 73% of the magnetic fields with flux density largerthan 2 Gauss is negative polarity, and 95% of the magnetic fields is negative,if we only measure the fields with their flux density larger than 20 Gauss. Ourresults display that in a coronal hole, stronger fields is occupied by onepredominant polarity; however the majority of weaker fields, occupied by theother polarity.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We investigate the detailed dynamics of multidimensional Hamiltonian systemsby studying the evolution of volume elements formed by unit deviation vectorsabout their orbits. The behavior of these volumes is strongly influenced by theregular or chaotic nature of the motion, the number of deviation vectors, theirlinear (in)dependence and the spectrum of Lyapunov exponents. The differenttime evolution of these volumes can be used to identify rapidly and efficientlythe nature of the dynamics, leading to the introduction of quantities thatclearly distinguish between chaotic behavior and quasiperiodic motion on$N$-dimensional tori. More specifically we introduce the Generalized AlignmentIndex of order $k$ (GALI$_k$) as the volume of a generalized parallelepiped,whose edges are $k$ initially linearly independent unit deviation vectors fromthe studied orbit whose magnitude is normalized to unity at every time step.The GALI$_k$ is a generalization of the Smaller Alignment Index (SALI)(GALI$_2$ $\\propto$ SALI). However, GALI$_k$ provides significantly moredetailed information on the local dynamics, allows for a faster and clearerdistinction between order and chaos than SALI and works even in cases where theSALI method is inconclusive.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The sub-millimetre wavelength regime is perhaps the most poorly explored overlarge areas of the sky, despite the considerable effort that has been expendedin making deep maps over small regions. As a consequence the properties of thesub-millimetre sky as a whole, and of rare bright objects in particular,remains largely unknown. Here we describe a forthcoming survey (the SCUBA-2``All-Sky'' Survey, or SASSy) designed to address this issue by making alarge-area map of approximately one-fifth of the sky visible from the JCMT(4800 square degrees) down to a 1 sigma noise level of 30 mJy/beam. This mapforms the pilot for a much larger survey, which will potentially map theremaining sky visible from the JCMT, with the region also visible to ALMA as apriority. SASSy has been awarded 500 hours for the 4800 square degree pilotphase and will commence after the commissioning of SCUBA-2, expected in early2008.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Phylogenetic mixtures model the inhomogeneous molecular evolution commonlyobserved in data. The performance of phylogenetic reconstruction methods wherethe underlying data is generated by a mixture model has stimulated considerablerecent debate. Much of the controversy stems from simulations of mixture modeldata on a given tree topology for which reconstruction algorithms output a treeof a different topology; these findings were held up to show the shortcomingsof particular tree reconstruction methods. In so doing, the underlyingassumption was that mixture model data on one topology can be distinguishedfrom data evolved on an unmixed tree of another topology given enough data andthe ``correct'' method. Here we show that this assumption can be false. Forbiologists our results imply that, for example, the combined data from twogenes whose phylogenetic trees differ only in terms of branch lengths canperfectly fit a tree of a different topology.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Computational asymmetry, i.e., the discrepancy between the complexity oftransformations and the complexity of their inverses, is at the core of one-waytransformations. We introduce a computational asymmetry function that measuresthe amount of one-wayness of permutations. We also introduce the word-lengthasymmetry function for groups, which is an algebraic analogue of computationalasymmetry. We relate boolean circuits to words in a Thompson monoid, over afixed generating set, in such a way that circuit size is equal to word-length.Moreover, boolean circuits have a representation in terms of elements of aThompson group, in such a way that circuit size is polynomially equivalent toword-length. We show that circuits built with gates that are not constrained tohave fixed-length inputs and outputs, are at most quadratically more compactthan circuits built from traditional gates (with fixed-length inputs andoutputs). Finally, we show that the computational asymmetry function is closelyrelated to certain distortion functions: The computational asymmetry functionis polynomially equivalent to the distortion of the path length in Schreiergraphs of certain Thompson groups, compared to the path length in Cayley graphsof certain Thompson monoids. We also show that the results of Razborov andothers on monotone circuit complexity lead to exponential lower bounds oncertain distortions.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Let $r>2$ and $\\sigma\\in(0,r-1)$ be integers. We require $t<2s$, where$t=2^{\\sigma+1}-1$ and $s=2^{r-\\sigma-1}$. Generalizing a known$\\{K_4,T_{6,3}\\}$-ultrahomogenous graph $G_3^1$, we find that a finite,connected, undirected, arc-transitive graph $G_r^\\sigma$ exists each of whoseedges is shared by just two maximal subgraphs, namely a clique $X_0=K_{2s}$ anda $t$-partite regular-Tur\\'an graph $X_1=T_{st,t}$ on $s$ vertices per part.Each copy $Y$ of $X_i$ ($i=0,1$) in $G_r^\\sigma$ shares each edge with just onecopy of $X_{1-i}$ and all such copies of $X_{1-i}$ are pairwise distinct.Moreover, $G_r^\\sigma$ is an edge-disjoint union of copies of $X_i$, for$i=0,1$. We prove that $G_r^\\sigma$ is $\\{K_{2s},T_{st,t}\\}$-homogeneous if$t<2s$, and just $\\{T_{st,t}\\}$-homogeneous otherwise, meaning that there is anautomorphism of $G_r^\\sigma$ between any two such copies of $X_i$ relating twopreselected arcs.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Author offers and researched the new and revolutionary inflatableelectrostatic AB space towers (mast, new space elevator) up to one hundredtwenty thousands kilometers (or more) in height. The main innovation is fillingthe tower by electron gas, which can create pressure up one atmosphere, hasnegligible small weight and surprising properties.  The suggested mast has following advantages in comparison with conventionalspace elevator: 1. Electrostatic AB tower may be built from Earth surfacewithout the employment of any rockets. That decreases the cost of electrostaticmast by thousands of times. 2. One can have any height and has a big controlload capacity. 3. Electrostatic tower can have the height of a geosynchronousorbit (36,000 km) WITHOUT the additional top cable as the space elevator (up120,000 - 160,000 km) and counterweight (equalizer) of hundreds of tons. 4. Theoffered mast has less total mass than conventional space elevator. 5. Theoffered tower can have the high-speed electrostatic climbers moved byhigh-voltage electricity from Earth's surface. 6. The electrostatic mast canbend in any needed direction when we give the necessary electric voltage in therequired parts of the extended mast. 7. Control mast has stability for anyaltitude. Three projects 100 km, 36,000km (GEO), 120,000 km are computed andpresented.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present a model improving the two-angle model for interphase chromatin(E2A model). This model takes into account the cylindrical shape of the histoneoctamers, the H1 histones in front of the nucleosomes and the vertical distance$d$ between the in and outgoing DNA strands. Factoring these chromatin featuresin, one gets essential changes in the chromatin phase diagram: Not only theshape of the excluded-volume borderline changes but also the vertical distance$d$ has a dramatic influence on the forbidden area. Furthermore, we examinedthe influence of H1 defects on the properties of the chromatin fiber. Thus wepresent two possible strategies for chromatin compaction: The use of very densestates in the phase diagram in the gaps in the excluded volume borderline ormissing H1 histones which can lead to very compact fibers. The chromatin fibermight use both of these mechanisms to compact itself at least locally. Linedensities computed within the model coincident with the experimental values.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We characterize the crystalline silicate content and spatial distribution ofsmall dust grains in a large sample of protoplanetary disks in theTaurus-Auriga young cluster, using Spitzer Space Telescope mid-infraredspectra. In turn we use the results to analyze the evolution of structure andcomposition of these 1-2 Myr-old disks around Solar- and later-type youngstars, and test the standard models of dust processing which result in theconversion of originally amorphous dust into minerals. We find strong evidenceof evolution of the dust crystalline mass fraction in parallel with that of thestructure of the disks, in the sense that increasing crystalline mass fractionis strongly linked to dust settling to the disk midplane. We also confirm thatthe crystalline silicates are confined to small radii, r < 10 AU. However, wesee no significant correlation of crystalline mass fraction with stellar massor luminosity, stellar accretion rate, disk mass, or disk/star mass ratio, aswould be expected in the standard models of dust processing based uponphoto-evaporation and condensation close to the central star,accretion-heating-driven annealing at r < 1 AU, or spiral-shock heating at r <10 AU, with or without effective radial mixing mechanisms. Either anothergrain-crystallizing mechanism dominates over these, or another process must beat work within the disks to erase the correlations they produce. We propose oneof each sort that seem to be worth further investigation, namely X-ray heatingand annealing of dust grains, and modulation of disk structure bygiant-planetary formation and migration.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "I consider the question of the interaction between a QCD string and the spinof a quark or an antiquark on whose worldline the string terminates. Theproblem is analysed from the point of view of a string representation for theexpectation value of a Wilson loop for a spin-half particle. A stringrepresentation of the super Wilson loop is obtained starting from an effectivestring representation of a Wilson Loop. The action obtained in this manner isinvariant under a worldline supersymmetry and has a boundary term whichcontains the spin-string interaction. For rectangular loops the spin-stringinteraction vanishes and there is no spin-spin term in the resulting heavyquark potential. On the other hand if an allowance is made for the finiteintrinsic thickness of the flux-tube, by assuming that the spin-stringinteraction takes place not just at the boundary of the string world-sheet butextends to a distance of the order of the intrinsic thickness of the flux tube,then we do obtain a spin-spin interaction which falls as the fifth power of thedistance. Such a term was previously suggested by Kogut and Parisi in thecontext of a flux-tube model of confinement.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Production of $D_{sJ}$(2317) mesons in relativistic heavy ion collisions atRHIC is studied. Using the quark coalescence model, we first determine theinitial number of $D_{sJ}$(2317) mesons produced during hadronization ofcreated quark-gluon plasma. The predicted $D_{sJ}$(2317) abundance dependssensitively on the quark structure of the $D_{sJ}$(2317) meson. Anorder-of-magnitude larger yield is obtained for a conventional two-quark thanfor an exotic four-quark $D_{sJ}$(2317) meson. To include the hadronic effecton the $D_{sJ}$(2317) meson yield, we have evaluated the absorption crosssections of the $D_{sJ}$(2317) meson by pion, rho, anti-kaon, and vectoranti-kaon in a phenomenological hadronic model. Taking into consideration theabsorption and production of $D_{sJ}$(2317) mesons during the hadronic stage ofheavy ion collisions via a kinetic model, we find that the final yield of$D_{sJ}$(2317) mesons remains sensitive to its initial number produced from thequark-gluon plasma, providing thus the possibility of studying the quarkstructure of the $D_{sJ}$(2317) meson and its production mechanism inrelativistic heavy ion collisions.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We investigate the growth of half metallic phase in a ferromagnetic materialusing state-of-the-art full potential linearized augmented plane wave method.To address the issue, we have substituted Ti at the Ru-sites in SrRuO3, whereSrRuO3 is a ferromagnetic material. Calculated results establish Ti4+ valencestates (similar to SrTiO3), which was predicted experimentally. Thus, Tisubstitution dilutes the Ru-O-Ru connectivity, which is manifested in thecalculated results in the form of significant band narrowing leading to finitegap between t2g and eg bands. At 75% substitution, a large gap (> 2 eV) appearsat the Fermi level, e_F in the up spin density of states, while the down spinstates contributes at e_F characterizing the system a half-metallicferromagnet. The t2g - eg gap can be tailored judiciously by tuning Ticoncentrations to minimize thermal effects, which is often the major bottleneckto achieve high spin polarization at elevated temperatures in other materials.This study, thus, provides a novel but simple way to fabricate half-metallicityin ferromagnetic materials, which are potential candidates for spin-basedtechnology.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The physical interpretation of scattering line polarization offers a noveldiagnostic window for exploring the thermal and magnetic structure of the quietregions of the solar atmosphere. Here we evaluate the impact of isotropiccollisions with neutral hydrogen atoms on the scattering polarization signalsof the 13 lines of multiplet 42 of Ti I and on those of the K line and of theIR triplet of Ca II, with emphasis on the collisional transfer rates betweennearby J-levels. To this end, we calculate the linear polarization produced byscattering processes considering realistic multilevel models and solving thestatistical equilibrium equations for the multipolar components of the atomicdensity matrix. We confirm that the lower levels of the 13 lines of multiplet42 of Ti I are completely depolarized by elastic collisions. We find thatupper-level collisional depolarization turns out to have an unnoticeable impacton the emergent linear polarization amplitudes, except for the ${\\lambda 4536$line for which it is possible to notice a rather small depolarization caused bythe collisional transfer rates. Concerning the Ca II lines, we show that thecollisional rates play no role on the polarization of the upper level of the Kline, while they have a rather small depolarizing effect on the atomicpolarization of the metastable lower levels of the Ca II IR triplet.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present results of a 20 ksec X-ray observation of the Wolf-Rayet (WR)binary system WR 147 obtained with XMM-Newton. Previous studies have shown thatthis system consists of a nitrogen-type WN8 star plus an OB companion whosewinds are interacting to produce a colliding wind shock. X-ray spectra from thepn and MOS detectors confirm the high extinction reported from IR studies andreveal hot plasma including the first detection of the Fe K-alpha line complexat 6.67 keV. Spectral fits with a constant-temperature plane-parallel shockmodel give a shock temperature kT(shock) = 2.7 keV [T(shock) ~ 31 MK], close tobut slightly hotter than the maximum temperature predicted for a colliding windshock. Optically thin plasma models suggest even higher temperatures, which arenot yet ruled out. The X-ray spectra are harder than can be accounted for using2D numerical colliding wind shock models based on nominal mass-loss parameters.Possible explanations include: (i) underestimates of the terminal wind speedsor wind abundances, (ii) overly simplistic colliding wind models, or (iii) thepresence of other X-ray emission mechanisms besides colliding wind shocks.Further improvement of the numerical models to include potentially importantphysics such as non-equilibrium ionization will be needed to rigorously testthe colliding wind interpretation.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We investigate non-perturbative features of a three-dimensional Abelian Higgsmodel with singly- and doubly-charged scalar fields coupled to a single compactAbelian gauge field. The model is pretending to describe various planar systemsof strongly correlated electrons such as high-Tc superconductivity in theoverdoped regime and exotic materials possessing excitations withfractionalized quantum numbers. The complicated phase structure of the model isstudied thoroughly using numerical tools and analytical arguments. In thethree-dimensional space of coupling parameters we identify the Fermi liquid,the spin gap, the superconductor and the strange metallic phases. The behaviorof three kinds of topological defects -- holon and spinon vortices andmonopoles - is explored in various phases. We also observe a new effect, thestrong enhancement of the phase transition strength reflected in a lower orderof the transition: at sufficiently strong gauge coupling the two second orderphase transitions -- corresponding to spinon-pair and holon condensation lines- join partially in the phase diagram and become a first order phase transitionin that region. The last observation may have an analogue in QuantumChromodynamics at non-zero temperature and finite baryon density. We argue thatat sufficiently large baryon density the finite-temperature transition betweenthe (3-flavor paired) color superconducting phase and the quark-gluon plasmaphases should be much stronger compared with the transition between 2-flavorpaired and 3-flavor paired superconducting phases.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present the results of a uniform analysis of the soft X-ray spectra offifteen type I AGN observed with the high resolution X-ray gratings on board\\emph{Chandra}. We found that ten of the fifteen AGN exhibit signatures of anintrinsic ionized absorber. The absorbers are photoionized and outflowing, withvelocities in the range $\\sim 10^{1}-10^{3}$ km $\\rm{s}^{-1}$. The columndensity of the warm absorbing gas is $\\sim 10^{20-23} \\rm{cm}^{-2}$. Nine ofthe ten AGN exhibiting warm absorption are best--fit by multiple ionizationcomponents and three of the ten AGN \\emph{require} multiple kinematiccomponents. The warm absorbing gas in our AGN sample has a wide range ofionization parameter, spanning roughly four orders of magnitude ($\\xi \\sim10^{0-4}$ ergs cm $\\rm{s}^{-1}$) in total, and often spanning three orders ofmagnitude in the same gas. Warm absorber components with ionization parameter$\\xi<10$ generate an unresolved transition array due to Fe in seven of the tenAGN exhibiting warm absorption. These low ionization state absorbers may alsocarry away the largest mass outflows from the AGN. The mass outflow ratedepends critically on the volume filling factor of the gas, which cannot yet bedirectly measured. However, upper limits on the mass outflow ratesfor fillingfactors of unity can be much greater than the expected accretion rate onto thecentral supermassive black hole and filling factors as small as 1% can giveoutflow rates comparable to the accretion rate. There appears to be a gap inthe outflow velocities in our sample between $\\sim 300-500$ km $\\rm{s}^{-1}$,the origin of which is not clear. The outflow components with velocities belowthis gap tend to be associated with lower column densities than those withvelocities above the gap.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We introduce a new spinfoam vertex to be used in models of 4d quantum gravitybased on SU(2) and SO(4) BF theory plus constraints. It can be seen as theconventional vertex of SU(2) BF theory, the 15j symbol, in a particular basisconstructed using SU(2) coherent states. This basis makes the geometricinterpretation of the variables transparent: they are the vectors normal to thetriangles within each tetrahedron. We study the condition under which thesestates can be considered semiclassical, and we show that the semiclassical onesdominate the evaluation of quantum correlations. Finally, we describe how theconstraints reducing BF to gravity can be directly written in terms of the newvariables, and how the semiclassicality of the states might improveunderstanding the correct way to implement the constraints.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "A model for charge transfer mechanism in YBa2Cu3O6+x high-Tc cuprate based oncritical chain length concept is proposed to account for 60K and 90K plateausin Tc(x) dependence. It has been shown, when the statistics of CuO chainformation was described in terms of two dimensional asymmetric next-to-nearestneighbor Ising (ASYNNNI) model, that at any constant temperature below the topof OII phase there exists a uniquely defined value of critical chain lengthlcr(T) that yields a constant doping p(x)=const over the regime of OII phase(related to 60K plateau of Tc(x)), while 90K plateau coincides with themonotonously increasing p(x) over optimal doping level p=0.16 in the regime ofOI phase. Short length chains (l<lcr(T)), together with the first lcr(T)-2holes in longer chains (l>lcr(T)), are taken as not capable of attractingelectrons from CuO2 planes.. It is shown that only a part (41%) of theremaining l-lcr(T)+1 holes in the long chains can capture electrons. Theresults obtained indicate that the ASYNNNI model and two-plateaus-like behaviorof Tc(x) in YBa2Cu3O6+x are closely connected.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Gravitational lenses on galaxy scales are plausibly modelled as havingellipsoidal symmetry and a universal dark matter density profile, with a Sersicprofile to describe the distribution of baryonic matter. Predicting all lensingeffects requires knowledge of the total lens potential: in this work we giveanalytic forms for that of the above hybrid model. Emphasising that complexlens potentials can be constructed from simpler components in linearcombination, we provide a recipe for attaining elliptical symmetry in eitherprojected mass or lens potential. We also provide analytic formulae for thelens potentials of Sersic profiles for integer and half-integer index. We thenpresent formulae describing the gravitational lensing effects due tosmoothly-truncated universal density profiles in cold dark matter model. Forour isolated haloes the density profile falls off as radius to the minus fifthor seventh power beyond the tidal radius, functional forms that allow allorders of lens potential derivatives to be calculated analytically, whileensuring a non-divergent total mass. We show how the observables predicted bythis profile differ from that of the original infinite-mass NFW profile.Expressions for the gravitational flexion are highlighted. We show howdecreasing the tidal radius allows stripped haloes to be modelled, providing aframework for a fuller investigation of dark matter substructure in galaxiesand clusters. Finally we remark on the need for finite mass halo profiles whendoing cosmological ray-tracing simulations, and the need for readily-calculablehigher order derivatives of the lens potential when studying catastrophes instrong lenses.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The presence of dust at high redshift requires efficient condensation ofgrains in SN ejecta, in accordance with current theoretical models. Yet,observations of the few well studied SNe and SN remnants imply condensationefficiencies which are about two orders of magnitude smaller. Motivated by thistension, we have (i) revisited the model of Todini & Ferrara (2001) for dustformation in the ejecta of core collapse SNe and (ii) followed, for the firsttime, the evolution of newly condensed grains from the time of formation totheir survival - through the passage of the reverse shock - in the SN remnant.We find that 0.1 - 0.6 M_sun of dust form in the ejecta of 12 - 40 M_sunstellar progenitors. Depending on the density of the surrounding ISM, between2-20% of the initial dust mass survives the passage of the reverse shock, ontime-scales of about 4-8 x 10^4 yr from the stellar explosion. Sputtering bythe hot gas induces a shift of the dust size distribution towards smallergrains. The resulting dust extinction curve shows a good agreement with thatderived by observations of a reddened QSO at z =6.2. Stochastic heating ofsmall grains leads to a wide distribution of dust temperatures. This supportsthe idea that large amounts (~ 0.1 M_sun) of cold dust (T ~ 40K) can be presentin SN remnants, without being in conflict with the observed IR emission.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We report the detection of five Jovian mass planets orbiting high metallicitystars. Four of these stars were first observed as part of the N2K program andexhibited low RMS velocity scatter after three consecutive observations.However, follow-up observations over the last three years now reveal thepresence of longer period planets with orbital periods ranging from 21 days toa few years. HD 11506 is a G0V star with a planet of \\msini = 4.74 \\mjup in a3.85 year orbit. HD 17156 is a G0V star with a 3.12 \\mjup planet in a 21.2 dayorbit. The eccentricity of this orbit is 0.67, one of the highest known for aplanet with a relatively short period. The orbital period for this planetplaces it in a region of parameter space where relatively few planets have beendetected. HD 125612 is a G3V star with a planet of \\msini = 3.5 \\mjup in a 1.4year orbit. HD 170469 is a G5IV star with a planet of \\msini = 0.67 \\mjup in a3.13 year orbit. HD 231701 is an F8V star with planet of 1.08 \\mjup in a 142day orbit. All of these stars have supersolar metallicity. Three of the fivestars were observed photometrically but showed no evidence of brightnessvariability. A transit search conducted for HD 17156 was negative but coveredonly 25% of the search space and so is not conclusive.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "N-body simulations give us a rough idea of how the shape of a simulatedobject appears in three-dimensional space. From an observational point of viewthis may give us a misleading picture. The faint stars may be the most commonstars in the system but the morphological information obtained by observationsof an object may be dominated by the color properties of the bright stars. Dueto dynamical effects, such as energy equipartition, different masses of starsmay populate different regions in the object. Since stars are evolving in massthe stellar evolution may also influence the dynamics of the system. Hence, ifone is interested in simulating what the morphology will look like through atelescope, one needs to simulate in addition evolving stars and weight them bytheir luminosity. Therefore we need to combine simulations of the dynamicalevolution and a stellar population synthesis at the same time. For thedynamical evolution part we use a parallel version of a direct N-body code,NBODY6++. This code also includes stellar evolution. We link the parametersfrom this stellar evolution routine to the BaSeL 2.0 stellar library. Forisolated clusters we found results assimilable to standard stellar populationsynthesis codes such as the PEGASE code. For clusters in a tidal field we foundthat the integrated colors become relatively bluer due to energy equipartitioneffects. In the time shortly before dissolution of the cluster the stellar M/Lratio becomes lower compared to isolated clusters. We compared the results ofour simulations to integrated spectra of galactic globular clusters. For thecluster NGC 1851 we found good agreement between simulation and observation.For extragalactic clusters in M81 and M31 we looked at medium band spectralenergy distributions and found for some clusters also a good agreement.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We show that the conditions which originate the spin and pseudospinsymmetries in the Dirac equation are the same that produce equivalent energyspectra of relativistic spin-1/2 and spin-0 particles in the presence of vectorand scalar potentials. The conclusions do not depend on the particular shapesof the potentials and can be important in different fields of physics. Whenboth scalar and vector potentials are spherical, these conditions forisospectrality imply that the spin-orbit and Darwin terms of either the uppercomponent or the lower component of the Dirac spinor vanish, making itequivalent, as far as energy is concerned, to a spin-0 state. In this case,besides energy, a scalar particle will also have the same orbital angularmomentum as the (conserved) orbital angular momentum of either the upper orlower component of the corresponding spin-1/2 particle. We point out a fewpossible applications of this result.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We study the application of AdS/CFT duality to longitudinal boost invariantBjorken expansion of QCD matter produced in ultrarelativistic heavy ioncollisions. As the exact (1+4)-dimensional bulk solutions for the(1+3)-dimensional boundary theory are not known, we investigate in detail the(1+1)-dimensional boundary theory, where the bulk is AdS_3 gravity. We find anexact bulk solution, show that this solution describes part of the spinlessBanados-Teitelboim-Zanelli (BTZ) black hole with the angular dimensionunwrapped, and use the thermodynamics of the BTZ hole to recover thetime-dependent temperature and entropy density on the boundary. Afterseparating from the holographic energy-momentum tensor a vacuum contribution,given by the extremal black hole limit in the bulk, we find that the boundaryfluid is an ideal gas in local thermal equilibrium. Including angular momentumin the bulk gives a boundary flow that is boost invariant but has a nonzerolongitudinal velocity with respect to the Bjorken expansion.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Star patterns, reminiscent of a wide range of diffusively controlled growthforms from snowflakes to Saffman-Taylor fingers, are ubiquitous features of icecovered lakes. Despite the commonality and beauty of these ``lake stars'' theunderlying physical processes that produce them have not been explained in acoherent theoretical framework. Here we describe a simple mathematical modelthat captures the principal features of lake-star formation; radial fingers of(relatively warm) water-rich regions grow from a central source and evolvethrough a competition between thermal and porous media flow effects in asaturated snow layer covering the lake. The number of star arms emerges from astability analysis of this competition and the qualitative features of thismeter-scale natural phenomena are captured in laboratory experiments.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present a detailed analysis of the Galaxy Stellar Mass Function ofgalaxies up to z=2.5 as obtained from the VVDS. We estimate the stellar massfrom broad-band photometry using 2 different assumptions on the galaxy starformation history and show that the addition of secondary bursts to acontinuous star formation history produces systematically higher (up to 40%)stellar masses. At low redshift (z=0.2) we find a substantial population oflow-mass galaxies (<10^9 Msun) composed by faint blue galaxies (M_I-M_K=0.3).In general the stellar mass function evolves slowly up to z=0.9 and moresignificantly above this redshift. Conversely, a massive tail is present up toz=2.5 and have extremely red colours (M_I-M_K=0.7-0.8). We find a decline withredshift of the overall number density of galaxies for all masses (59+-5% forM>10^8 Msun at z=1), and a mild mass-dependent average evolution(`mass-downsizing'). In particular our data are consistent with mild/negligible(<30%) evolution up to z=0.7 for massive galaxies (>6x10^10 Msun). For lessmassive systems the no-evolution scenario is excluded. A large fraction (>=50%)of massive galaxies have been already assembled and converted most of their gasinto stars at z=1, ruling out the `dry mergers' as the major mechanism of theirassembly history below z=1. This fraction decreases to 33% at z=2. Low-masssystems have decreased continuously in number and mass density (by a factor upto 4) from the present age to z=2, consistently with a prolonged mass assemblyalso at z<1.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present a comprehensive mass reconstruction of the rich galaxy cluster Cl0024+17 at z~0.4 from ACS data, unifying both strong- and weak-lensingconstraints. The weak-lensing signal from a dense distribution of backgroundgalaxies (~120 per square arcmin) across the cluster enables the derivation ofa high-resolution parameter-free mass map. The strongly-lensed objects tightlyconstrain the mass structure of the cluster inner region on an absolute scale,breaking the mass-sheet degeneracy. The mass reconstruction of Cl 0024+17obtained in such a way is remarkable. It reveals a ringlike dark mattersubstructure at r~75\" surrounding a soft, dense core at r~50\". We interpretthis peculiar sub-structure as the result of a high-speed line-of-sightcollision of two massive clusters 1-2 Gyr ago. Such an event is also indicatedby the cluster velocity distribution. Our numerical simulation with purelycollisionless particles demonstrates that such density ripples can arise byradially expanding, decelerating particles that originally comprised thepre-collision cores. Cl 0024+17 can be likened to the bullet cluster 1E0657-56,but viewed $along$ the collision axis at a much later epoch. In addition, weshow that the long-standing mass discrepancy for Cl 0024+17 between X-ray andlensing can be resolved by treating the cluster X-ray emission as coming from asuperposition of two X-ray systems. The cluster's unusual X-ray surfacebrightness profile that requires a two isothermal sphere description supportsthis hypothesis.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We combined sensitive near-infrared data obtained with ground-based imagerson the ESO NTT and VLT telescopes with space mid-infrared data acquired withthe IRAC imager on the Spitzer Space Telescope to calculate the extinction lawA_\\lambda/A_K as a function of \\lambda between 1.25 and 7.76 micron to anunprecedented depth in Barnard 59, a star forming, dense core located in thePipe Nebula. The ratios A_\\lambda/A_K were calculated from the slopes of thedistributions of sources in color-color diagrams \\lambda-K vs. H-K. Thedistributions in the color-color diagrams are fit well with single slopes toextinction levels of A_K ~ 7 (A_V ~ 59 mag). Consequently, there appears to beno significant variation of the extinction law with depth through the B59 lineof sight. However, when slopes are translated into the relative extinctioncoefficients A_\\lambda/A_K, we find an extinction law which departs from thesimple extrapolation of the near-infrared power law extinction curve, andagrees more closely with a dust extinction model for a cloud with a total toselective absorption R_V=5.5 and a grain size distribution favoring largergrains than those in the diffuse ISM. Thus, the difference we observe could bepossibly due to the effect of grain growth in denser regions. Finally, theslopes in our diagrams are somewhat less steep than those from the study ofIndebetouw et al. (2005) for clouds with lower column densities, and thisindicates that the extinction law between 3 and 8 micron might vary slightly asa function of environment.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We investigate the gravitational wake due to, and dynamical friction on, aperturber moving on a circular orbit in a uniform gaseous medium using asemi-analytic method. This work is a straightforward extension of Ostriker(1999) who studied the case of a straight-line trajectory. The circular orbitcauses the bending of the wake in the background medium along the orbit,forming a long trailing tail. The wake distribution is thus asymmetric, givingrise to the drag forces in both opposite (azimuthal) and lateral (radial)directions to the motion of the perturber, although the latter does notcontribute to orbital decay much. For subsonic motion, the density wake with aweak tail is simply a curved version of that in Ostriker and does not exhibitthe front-back symmetry. The resulting drag force in the opposite direction isremarkably similar to the finite-time, linear-trajectory counterpart. On theother hand, a supersonic perturber is able to overtake its own wake, possiblymultiple times, and develops a very pronounced tail. The supersonic tailsurrounds the perturber in a trailing spiral fashion, enhancing the perturbeddensity at the back as well as far front of the perturber. We provide thefitting formulae for the drag forces as functions of the Mach number, whoseazimuthal part is surprisingly in good agreement with the Ostriker's formula,provided Vp t=2 Rp, where Vp and Rp are the velocity and orbital radius of theperturber, respectively.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We report on a theoretical derivation of the electronic dielectric responseof semiconductor nanocrystals using a tight-binding framework. Extending to thenanoscale the Hanke and Sham approach [Phys. Rev. B 12, 4501 (1975)] developedfor bulk semiconductors, we show how local field effects can be included in thestudy of confined systems. A great advantage of this scheme is that of beingformulated in terms of localized orbitals and thus it requires very fewcomputational resources and times. Applications to the optical and screeningproperties of semiconductor nanocrystals are presented here and discussed.Results concerning the absorption cross section, the static polarizability andthe screening function of InAs (direct gap) and Si (indirect gap) nanocrystalscompare well to both first principles results and experimental data. We alsoshow that the present scheme allows us to easily go beyond the continuumdielectric model, based on the Clausius-Mossotti equation, which is frequentlyused to include the nanocrystal surface polarization. Our calculations indicatethat the continuum dielectric model, used in conjunction with a size dependentdielectric constant, underestimates the nanocrystal polarizability, leading toexceedingly strong surface polarization fields.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present in this paper three dynamic clustering techniques forObject-Oriented Databases (OODBs). The first two, Dynamic, Statistical &Tunable Clustering (DSTC) and StatClust, exploit both comprehensive usagestatistics and the inter-object reference graph. They are quite elaborate.However, they are also complex to implement and induce a high overhead. Thethird clustering technique, called Detection & Reclustering of Objects (DRO),is based on the same principles, but is much simpler to implement. These threeclustering algorithm have been implemented in the Texas persistent object storeand compared in terms of clustering efficiency (i.e., overall performanceincrease) and overhead using the Object Clustering Benchmark (OCB). The resultsobtained showed that DRO induced a lighter overhead while still achievingbetter overall performance.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "In this paper we address the problem of finding the sensing capacity ofsensor networks for a class of linear observation models and a fixed SNRregime. Sensing capacity is defined as the maximum number of signal dimensionsreliably identified per sensor observation. In this context sparsity of thephenomena is a key feature that determines sensing capacity. Precluding the SNRof the environment the effect of sparsity on the number of measurementsrequired for accurate reconstruction of a sparse phenomena has been widelydealt with under compressed sensing. Nevertheless the development there wasmotivated from an algorithmic perspective. In this paper our aim is to derivethese bounds in an information theoretic set-up and thus provide algorithmindependent conditions for reliable reconstruction of sparse signals. In thisdirection we first generalize the Fano's inequality and provide lower bounds tothe probability of error in reconstruction subject to an arbitrary distortioncriteria. Using these lower bounds to the probability of error, we derive upperbounds to sensing capacity and show that for fixed SNR regime sensing capacitygoes down to zero as sparsity goes down to zero. This means thatdisproportionately more sensors are required to monitor very sparse events. Ournext main contribution is that we show the effect of sensing diversity onsensing capacity, an effect that has not been considered before. Sensingdiversity is related to the effective \\emph{coverage} of a sensor with respectto the field. In this direction we show the following results (a) Sensingcapacity goes down as sensing diversity per sensor goes down; (b) Randomsampling (coverage) of the field by sensors is better than contiguous locationsampling (coverage).", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present numerical studies for finitely extensible nonlinear elastic (FENE)dumbbells which are dispersed in a turbulent plane shear flow at moderateReynolds number. The polymer ensemble is described on the mesoscopic level by aset of stochastic ordinary differential equations with Brownian noise. Thedynamics of the Newtonian solvent is determined by the Navier-Stokes equations.Momentum transfer of the dumbbells with the solvent is implemented by anadditional volume forcing term in the Navier-Stokes equations, such that bothcomponents of the resulting viscoelastic fluid are connected by a two-waycoupling. The dynamics of the dumbbells is given then by Newton's second law ofmotion including small inertia effects. We investigate the dynamics of the flowfor different degrees of dumbbell elasticity and inertia, as given byWeissenberg and Stokes numbers, respectively. For the parameters accessible inour study, the magnitude of the feedback of the polymers on the macroscopicproperties of turbulence remains small as quantified by the global energybudget and the Reynolds stresses. A reduction of the turbulent drag by up to20% is observed for the larger particle inertia. The angular statistics of thedumbbells shows an increasing alignment with the mean flow direction for both,increasing elasticity and inertia. This goes in line with a growing asymmetryof the probability density function of the transverse derivative of thestreamwise turbulent velocity component. We find that dumbbells get stretchedreferentially in regions where vortex stretching or bi-axial strain dominatethe local dynamics and topology of the velocity gradient tensor.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Inspired by a recent astro-ph posting, I propose a creation of an AlternativeHistory astro-ph archive (althistastro-ph). Such an archive would serve as afinal resting place for the various telescope (and possibly other) proposalsthat were not successful. As we all know, from both submitting proposals andalso from serving on various time allocation committees, many excellentproposals ``do not make it''. Creating such an AltHist archive would serve manygoals, including venting the frustration of the authors and also providingpossible amusement for the readers. These are worthy goals, but they alonewould not warrant creating such an archive. The truly useful role ofAltHistAstro-ph archive would be to match astronomers with unappreciated ideaswith other astronomers with underutilized resources, hopefully leading in somecases to resurrection of old proposals and resulting publications in theregular astro-ph archive. Given the possible danger of a low signal-to-noiseand possible confusion, a creation of a separate archive seems like a goodidea, although it should be noted that low signal-to-noise is achieved onastro-ph quite often already. Finally, I include my own excellent, but rejected(twice), HST proposal, as an example of a potential AltHistAstro-ph posting.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The $n$-dimensional complex hyperquadric is a compact complex algebraichypersurface defined by the quadratic equation in the $(n+1)$-dimensionalcomplex projective space, which is isometric to the real Grassmann manifold oforiented 2- planes and is a compact Hermitian symmetric space of rank 2. Inthis paper we study geometry of compact Lagrangian submanifolds in complexhyperquadrics from the viewpoint of the theory of isoparametric hypersurfacesin spheres. From this viewpoint we provide a classification theorem of compacthomogeneous Lagrangian submanifolds in complex hyperquadrics by using themoment map technique. Moreover we determine the Hamiltonian stability ofcompact minimal Lagrangian submanifolds embedded in complex hyperquadrics whichare obtained as Gauss images of isoparametric hypersurfaces in spheres with$g(=1,2,3)$ distinct principal curvatures.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "There is a large literature devoted to the problem of finding an optimal(min-cost) prefix-free code with an unequal letter-cost encoding alphabet ofsize. While there is no known polynomial time algorithm for solving itoptimally there are many good heuristics that all provide additive errors tooptimal. The additive error in these algorithms usually depends linearly uponthe largest encoding letter size.  This paper was motivated by the problem of finding optimal codes when theencoding alphabet is infinite. Because the largest letter cost is infinite, theprevious analyses could give infinite error bounds. We provide a new algorithmthat works with infinite encoding alphabets. When restricted to the finitealphabet case, our algorithm often provides better error bounds than the bestprevious ones known.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We show that observations of high-redshift Ly-alpha emitters (LAEs) have thepotential to provide definitive evidence for reionization in the near future.Using 200 Mpc radiative transfer simulations, we calculate the effect thatpatchy reionization has on the line profile, on the luminosity function, and,most interestingly, on the clustering of emitters for several realistic modelsof reionization. Reionization increases the measured clustering of emitters,and we show that this enhancement would be essentially impossible to attributeto anything other than reionization. Our results motivate looking for thesignature of reionization in existing LAE data. We find that for stellarreionization scenarios the angular correlation function of the 58 LAEs in theSubaru Deep Field z = 6.6 photometric sample is more consistent with a fullyionized universe (mean volume ionized fraction x_i = 1) than a universe withx_i < 0.5 at >2-sigma confidence level. Measurements in the next year on Subaruwill increase their z = 6.6 LAE sample by a factor of five and tighten theselimits. If the clustering signature of reionization is detected in a LAEsurvey, a comparison with a Lyman-break or a H-alpha survey in the same fieldwould confirm the reionization hypothesis. We discuss the optimal LAE surveyspecifications for detecting reionization, with reference to upcoming programs.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "A general {\\it ab-initio} and non-perturbative method to solve thetime-dependent Schr\\\"odinger equation (TDSE) for the interaction of a strongattosecond laser pulse with a general atom, i.e., beyond the models ofquasi-one-electron or quasi-two-electron targets, is described. The field-freeHamiltonian and the dipole matrices are generated using a flexible $B$-spline$R$-matrix method. This numerical implementation enables us to constructterm-dependent, non-orthogonal sets of one-electron orbitals for the bound andcontinuum electrons. The solution of the TDSE is propagated in time using theArnoldi-Lanczos method, which does not require the diagonalization of any largematrices. The method is illustrated by an application to the multi-photonexcitation and ionization of Ne atoms. Good agreement with $R$-matrix Floquetcalculations for the generalized cross sections for two-photon ionization isachieved.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Starting with a field theoretic approach in Minkowski space, thegravitational energy momentum tensor is derived from the Einstein equations ina straightforward manner. This allows to present them as {\\it accelerationtensor} = const. $\\times$ {\\it total energy momentum tensor}. For flat spacecosmology the gravitational energy is negative and cancels the material energy.In the relativistic theory of gravitation a bimetric coupling between theRiemann and Minkowski metrics breaks general coordinate invariance. The case ofa positive cosmological constant is considered. A singularity free version ofthe Schwarzschild black hole is solved analytically. In the interior thecomponents of the metric tensor quickly die out, but do not change sign,leaving the role of time as usual. For cosmology the $\\Lambda$CDM model iscovered, while there appears a form of inflation at early times. Here both thetotal energy and the zero point energy vanish.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Recently, an extension of the standard model based on ideas of Lee and Wickhas been discussed. This theory is free of quadratic divergences and hence hasa Higgs mass that is stable against radiative corrections. Here, we address thequestion of whether or not it is possible to couple very heavy particles, withmasses much greater than the weak scale, to the Lee-Wick standard model degreesof freedom and still preserve the stability of the weak scale. We show that inthe LW-standard model the familiar see-saw mechanism for generating neutrinomasses preserves the solution to the hierarchy puzzle provided by the higherderivative terms. The very heavy right handed neutrinos do not destabilize theHiggs mass. We give an example of new heavy degrees of freedom that woulddestabilize the hierarchy, and discuss a general mechanism for coupling otherheavy degrees of freedom to the Higgs doublet while preserving the hierarchy.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We establish the first hardness results for the problem of computing thevalue of one-round games played by a verifier and a team of provers who canshare quantum entanglement. In particular, we show that it is NP-hard toapproximate within an inverse polynomial the value of a one-round game with (i)quantum verifier and two entangled provers or (ii) classical verifier and threeentangled provers. Previously it was not even known if computing the valueexactly is NP-hard. We also describe a mathematical conjecture, which, if true,would imply hardness of approximation to within a constant.  We start our proof by describing two ways to modify classical multi-provergames to make them resistant to entangled provers. We then show that a strategyfor the modified game that uses entanglement can be ``rounded'' to one thatdoes not. The results then follow from classical inapproximability bounds. Ourwork implies that, unless P=NP, the values of entangled-prover games cannot becomputed by semidefinite programs that are polynomial in the size of theverifier's system, a method that has been successful for more restrictedquantum games.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "When a source emits a gravity-wave (GW) pulse over a short period of time,the leading edge of the GW signal is redshifted more than the inner boundary ofthe pulse. The GW pulse is distorted by the gravitational effect of theself-energy residing in between these shells. We illustrate this distortion forGW pulses from the final plunge of black hole (BH) binaries, leading to theevolution of the GW profile as a function of the radial distance from thesource. The distortion depends on the total GW energy released and the durationof the emission, scaled by the total binary mass, M. The effect should berelevant in finite box simulations where the waveforms are extracted within aradius of <~ 100M. For characteristic emission parameters at the final plungebetween binary BHs of arbitrary spins, this effect could distort the simulatedGW templates for LIGO and LISA by a fraction of 0.001. Accounting for the wavedistortion would significantly decrease the waveform extraction errors innumerical simulations.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Determinations of beryllium abundance in stars, together with lithium,provide a key tool to investigate the so far poorly understood extra-mixingprocesses at work in stellar interiors. We measured Be in three openclusters,complementing existing Be surveys, and aiming at gathering a morecomplete empirical scenario of the evolution of Be as a function of stellar ageand temperature. Specifically, we analyzed VLT/UVES spectra of members of NGC2516, the Hyades, and M 67 to determine their Be and Li abundances. In thefirst two clusters we focused on stars cooler than 5400 K, while the M 67sample includes stars warmer than 6150 K, as well as two subgiants and two bluestragglers. We also computed the evolution of Be for a 0.9 Mo star based onstandard evolutionary models. We find different emprical behaviours for starsin different temperature bins and ages. Stars warmer than 6150 K show Bedepletion and follow a Be vs. Li correlation while Be is undepleted in stars inthe ~6150-5600 K range. NGC 2516 members cooler than 5400 K have not depletedany Be, but older Hyades of similar temperature do show some depletion. Be isseverely depleted in the subgiants and blue stragglers. The results for warmstars are in agreement with previous studies, supporting the hypothesis thatmixing in this temperature regime is driven by rotation. The same holds for thetwo subgiants that have evolved from the \"Li gap\". This mechanism is insteadnot the dominant one for solar-type stars. We show that Be depletion of coolHyades cannot simply be explained by the effect of increasing depth of theconvective zone. Finally, the different Be content of the two blue stragglerssuggests that they have formed by two different processes (i.e., collisions vs.binary merging).", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Different types of superfluid ground states have been investigated in systemsof two species of fermions with Fermi surfaces that do not match. This study isrelevant for cold atomic systems, condensed matter physics and quark matter. Inthis paper we consider this problem in the case the fermionic quasi-particlescan transmute into one another and only their total number is conserved. We usea BCS approximation to study superconductivity in two-band metallic systemswith inter and intra-band interactions. Tuning the hybridization between thebands varies the mismatch of the Fermi surfaces and produces differentinstabilities. For inter-band attractive interactions we find a first ordernormal-superconductor and a homogeneous metastable phase with gaplessexcitations. In the case of intra-band interactions, the transition from thesuperconductor to the normal state as hybridization increases is continuous andassociated with a quantum critical point. The case when both interactions arepresent is also considered.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We obtain a first order differential equation for the driving function of thechordal Loewner differential equation in the case where the domain is slit by acurve which is a trajectory arc of certain quadratic differentials. Inparticular this includes the case when the curve is a path on the square,triangle or hexagonal lattice in the upper halfplane or, indeed, in any domainwith boundary on the lattice. We also demonstrate how we use this to calculatethe driving function numerically. Equivalent results for other variants of theLoewner differential equation are also obtained: Multiple slits in the chordalLoewner differential equation and the radial Loewner differential equation. Themethod also works for other versions of the Loewner differential equation. Theproof of our formula uses a generalization of Schwarz-Christoffel mapping todomains bounded by trajectory arcs of rotations of a given quadraticdifferential that is of interest in its own right.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "An epidemic multi-strain model with temporary cross-immunity shows chaos,even in a previously unexpected parameter region. Especially dengue fevermodels with strong enhanced infectivity on secondary infection have previouslyshown deterministic chaos motivated by experimental findings ofantibody-dependent-enhancement (ADE). Including temporary cross-immunity insuch models, which is common knowledge among field researchers in dengue, wefind a deterministically chaotic attractor in the more realistic parameterregion of reduced infectivity on secondary infection (''inverse ADE'' parameterregion). This is realistic for dengue fever since on second infection peopleare more likely to be hospitalized, hence do not contribute to the force ofinfection as much as people with first infection.  Our finding has wider implications beyond dengue in any multi-strainepidemiological systems with altered infectivity upon secondary infection,since we can relax the condition of rather high infectivity on secondaryinfection previously required for deterministic chaos. For dengue the findingof wide ranges of chaotic attractors open new ways to analysis of existing datasets.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present a detailed analysis of the prompt and afterglow emission of GRB050410 and GRB 050412 detected by Swift for which no optical counterpart wasobserved. The 15-150 keV energy distribution of the GRB 050410 prompt emissionshows a peak energy at 53 keV. The XRT light curve of this GRB decays as apower law with a slope of alpha=1.06+/-0.04. The spectrum is well reproduced byan absorbed power law with a spectral index Gamma_x=2.4+/-0.4 and a low energyabsorption N_H=4(+3;-2)x10^21 cm^(-2) which is higher than the Galactic value.The 15-150 keV prompt emission in GRB 050412 is modelled with a hard(Gamma=0.7+/-0.2) power law. The XRT light curve follows a broken power lawwith the first slope alpha_1=0.7+/-0.4, the break time T_break=254(-41;+79) sand the second slope alpha_2=2.8(-0.8;+0.5). The spectrum is fitted by a powerlaw with spectral index Gamma_x=1.3+/-0.2 which is absorbed at low energies bythe Galactic column. The GRB 050410 afterglow reveals the expectedcharacteristics of the third component of the canonical Swift light curve.Conversely, a complex phenomenology was detected in the GRB 050412 because ofthe presence of the very early break. The light curve in this case can beinterpreted as being the last peak of the prompt emission. The two burstspresent tight upper limits for the optical emission, however, neither of themcan be clearly classified as dark. For GRB 050410, the suppression of theoptical afterglow could be attributed to a low density interstellar mediumsurrounding the burst. For GRB 050412, the evaluation of the darkness is moredifficult due to the ambiguity in the extrapolation of the X-ray afterglowlight curve.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "High-resolution spectroscopy of U Gem was obtained during quiescence. We didnot find a hot spot or gas stream around the outer boundaries of the accretiondisk. Instead, we detected a strong narrow emission near the location of thesecondary star. We measured the radial velocity curve from the wings of thedouble-peaked H$\\alpha$ emission line, and obtained a semi-amplitude value thatis in excellent agreement with the obtained from observations in theultraviolet spectral region by Sion et al. (1998). We present also a new methodto obtain K_2, which enhances the detection of absorption or emission featuresarising in the late-type companion. Our results are compared with publishedvalues derived from the near-infrared NaI line doublet. From a comparison ofthe TiO band with those of late type M stars, we find that a best fit isobtained for a M6V star, contributing 5 percent of the total light at thatspectral region. Assuming that the radial velocity semi-amplitudes reflectaccurately the motion of the binary components, then from our results: K_em =107+/-2 km/s; K_abs = 310+/-5 km/s, and using the inclination angle given byZhang & Robinson(1987); i = 69.7+/-0.7, the system parameters become: M_WD =1.20+/-0.05 M_sun,; M_RD = 0.42+/-0.04 M_sun; and a = 1.55+/- 0.02 R_sun. Basedon the separation of the double emission peaks, we calculate an outer diskradius of R_out/a ~0.61, close to the distance of the inner Lagrangian pointL_1/a~0.63. Therefore we suggest that, at the time of observations, theaccretion disk was filling the Roche-Lobe of the primary, and that the matterleaving the L_1 point was colliding with the disc directly, producing the hotspot at this location.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Rotating deformed neutron stars are important potential sources forgroundbased gravitational-wave interferometers such as LIGO, GE0600 and VIRGO.One mechanism that may lead to significant non-asymmetries is the internalmagnetic field. It is well known that a magnetic star will not be sphericaland, if the magnetic axis is not aligned with the spin axis, the deformationwill lead to the emission of gravitational waves. The aim of this paper is todevelop a formalism that would allow us to model magnetically deformed stars,using both realistic equations of state and field configurations. As a firststep, we consider a set of simplified model problems. Focusing on dipolarfields, we determine the internal magnetic field which is consistent with agiven neutron star model. We then calculate the associated deformation. Weconclude by discussing the relevance of our results for currentgravitational-wave detectors and future prospects.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Alexander B. Medvinsky \\emph{et al} [A. B. Medvinsky, I. A. Tikhonova, R. R.Aliev, B.-L. Li, Z.-S. Lin, and H. Malchow, Phys. Rev. E \\textbf{64}, 021915(2001)] and Marcus R. Garvie \\emph{et al} [M. R. Garvie and C. Trenchea, SIAMJ. Control. Optim. \\textbf{46}, 775-791 (2007)] shown that the minimalspatially extended reaction-diffusion model of phytoplankton-zooplankton canexhibit both regular, chaotic behavior, and spatiotemporal patterns in a patchyenvironment. Based on that, the spatial plankton model is furtherlyinvestigated by means of computer simulations and theoretical analysis in thepresent paper when its parameters would be expected in the case of mixedTuring-Hopf bifurcation region. Our results show that the spiral waves exist inthat region and the spatiotemporal chaos emerge, which arise from the far-fieldbreakup of the spiral waves over large ranges of diffusion coefficients ofphytoplankton and zooplankton. Moreover, the spatiotemporal chaos arising fromthe far-field breakup of spiral waves does not gradually involve the wholespace within that region. Our results are confirmed by means of computationspectra and nonlinear bifurcation of wave trains. Finally, we give someexplanations about the spatially structured patterns from the community level.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "In the bootstrap percolation model, sites in an L by L square are initiallyinfected independently with probability p. At subsequent steps, a healthy sitebecomes infected if it has at least 2 infected neighbours. As(L,p)->(infinity,0), the probability that the entire square is eventuallyinfected is known to undergo a phase transition in the parameter p log L,occurring asymptotically at lambda = pi^2/18. We prove that the discrepancybetween the critical parameter and its limit lambda is at least Omega((logL)^(-1/2)). In contrast, the critical window has width only Theta((logL)^(-1)). For the so-called modified model, we prove rigorous explicit boundswhich imply for example that the relative discrepancy is at least 1% even whenL = 10^3000. Our results shed some light on the observed differences betweensimulations and rigorous asymptotics.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The tilt modulus of a defective Abrikosov vortex lattice pinned by materialline defects is computed using the boson analogy. It tends to infinity at longwavelength, which yields a Bose glass state that is robust to the addition ofweak point-pinning centers, and which implies a restoring force per vortex linefor rigid translations about mechanical equilibrium that is independent ofmagnetic field. It also indicates that the Bose glass state breaks into piecesalong the direction of the correlated pinning centers if the latter have finitelength. The critical current is predicted to crossover from two dimensional tothree dimensional behavior as a function of sample thickness along thecorrelated pinning centers in such case. That crossover notably can occur at afilm thickness that is much larger than that expected from point pins ofcomparable strength. The above is compared to the dependence on thickness shownby the critical current in certain films of high-temperature superconductorscurrently being developed for wire technology.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We address two issues in the thermodynamic model for nuclear disassembly.Surprisingly large differences in results for specific heat were seen inpredictions from the canonical and grand canonical ensembles when the nuclearsystem passes from liquid-gas co-existence to the pure gas phase. We are ableto pinpoint and understand the reasons for such and other discrepancies whenthey appear. There is a subtle but important difference in the physicsaddressed in the two models. In particular if we reformulate the parameters inthe canonical model to better approximate the physics addressed in the grandcanonical model, calculations for observables converge. Next we turn to theissue of bimodality in the probability distribution of the largest fragment inboth canonical and grand canonical ensembles. We demonstrate that thisdistribution is very closely related to average multiplicities. Therelationship of the bimodal distribution to phase transition is discussed.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The near-infrared integral field spectrograph SINFONI at the ESO VLT opens anew window for the study of central supermassive black holes. With a near-IRspatial resolution similar to HST optical and the ability to penetrate dust itprovides the possibility to explore the low-mass end of the M-sigma relation(sigma<120km/s) where so far very few black hole masses were measured withstellar dynamics. With SINFONI we observed the central region of thelow-luminosity elliptical galaxy NGC4486a at a spatial resolution of ~0.1arcsecin the K band. The stellar kinematics was measured with a maximum penalisedlikelihood method considering the region around the CO absorption band heads.We determined a black hole mass of M_BH=1.25^{+0.75}_{-0.79} x 10^7 M_sun (90%C.L.) using the Schwarzschild orbit superposition method including the full2-dimensional spatial information. This mass agrees with the predictions of theM-sigma relation, strengthening its validity at the lower sigma end.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Propagation, transmission and reflection properties of linearly polarizedplane waves and arbitrarily short electromagnetic pulses in one-dimensionaldispersionless dielectric media possessing an arbitrary space-time dependenceof the refractive index are studied by using a two-component, highly symmetricversion of Maxwell's equations. The use of any slow varying amplitudeapproximation is avoided. Transfer matrices of sharp nonstationary interfacesare calculated explicitly, together with the amplitudes of all secondary wavesproduced in the scattering. Time-varying multilayer structures andspatiotemporal lenses in various configurations are investigated analyticallyand numerically in a unified approach. Several new effects are reported, suchas pulse compression, broadening and spectral manipulation of pulses by aspatiotemporal lens, and the closure of the forbidden frequency gaps with thesubsequent opening of wavenumber bandgaps in a generalized Bragg reflector.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We consider global and gravitational lensing properties of the recentlysuggested Einstein clusters of WIMPs as galactic dark matter halos. Beingtangential pressure dominated, Einstein clusters are strongly anisotropicsystems which can describe any galactic rotation curve by specifying theanisotropy. Due to this property, Einstein clusters may be considered as darkmatter candidates. We analyse the stability of the Einstein clusters againstboth radial and non-radial pulsations, and we show that the Einstein clustersare dynamically stable. With the use of the Buchdahl type inequalities foranisotropic bodies, we derive upper limits on the velocity of the particlesdefining the cluster. These limits are consistent with those obtained fromstability considerations. The study of light deflection shows that thegravitational lensing effect is slightly smaller for the Einstein clusters, ascompared to the singular isothermal density sphere model for dark matter.Therefore lensing observations may discriminate, at least in principle, betweenEinstein cluster and other dark matter models.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The environment of high-redshift galaxies is characterized by bothwind-driven outflowing gas and gravitationally infalling streams. Toinvestigate such galaxy-IGM interplay we have generated synthetic opticalabsorption line spectra piercing the volume surrounding a starbursting analogof a Lyman Break Galaxy selected in a $z \\approx 3$ output from a SPHsimulation, including a detailed treatment of mechanical feedback from winds.Distributions for several observable species (HI, CIII, CIV, SiII, SiIII, SiIV,OVI, OVII, and OVIII) have been derived by post-processing the simulationoutputs. The hot wind material is characterized by the presence ofhigh-ionization species such as OVI, OVII, and OVIII (the latter two observableonly in X-ray bands); the colder ($T<10^{5.5}$ K) infalling streams can beinstead identified by the combined presence of SiII, SiIII, and CIII opticalabsorption together with OVI that surrounds the cooler gas clumps. However,both line profile and Pixel Optical Depth analysis of the synthetic spectrashow that the intergalactic filament in which the wind-blowing galaxy isembedded produces absorption signatures that closely mimic those of the windenvironment. We conclude that may be difficult to clearly identify wind-blowinggalaxies and their complex gaseous environment at high redshift in optical QSOabsorption-line spectra based solely on the observed ion absorption patterns.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We study the effects of frustration in an antiferromagnetic film of FCClattice with Heisenberg spin model including an Ising-like anisotropy. MonteCarlo (MC) simulations have been used to study thermodynamic properties of thefilm. We show that the presence of the surface reduces the ground state (GS)degeneracy found in the bulk. The GS is shown to depend on the surface in-planeinteraction $J_s$ with a critical value at which ordering of type I coexistswith ordering of type II. Near this value a reentrant phase is found. Variousphysical quantities such as layer magnetizations and layer susceptibilities areshown and discussed. The nature of the phase transition is also studied byhistogram technique. We have also used the Green's function (GF) method for thequantum counterpart model. The results at low-$T$ show interesting effects ofquantum fluctuations. Results obtained by the GF method at high $T$ arecompared to those of MC simulations. A good agreement is observed.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "This paper addresses the performance of bit-interleaved coded multiplebeamforming (BICMB) [1], [2] with imperfect knowledge of beamforming vectors.Most studies for limited-rate channel state information at the transmitter(CSIT) assume that the precoding matrix has an invariance property under anarbitrary unitary transform. In BICMB, this property does not hold. On theother hand, the optimum precoder and detector for BICMB are invariant under adiagonal unitary transform. In order to design a limited-rate CSIT system forBICMB, we propose a new distortion measure optimum under this invariance. Basedon this new distortion measure, we introduce a new set of centroids and employthe generalized Lloyd algorithm for codebook design. We provide simulationresults demonstrating the performance improvement achieved with the proposeddistortion measure and the codebook design for various receivers with lineardetectors. We show that although these receivers have the same performance forperfect CSIT, their performance varies under imperfect CSIT.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We discuss a universality property of any covariant field theory inspace-time expanded around pp-wave backgrounds. According to this property thespace-time lagrangian density evaluated on a restricted set of fieldconfigurations, called universal sector, turns out to be same around all thepp-waves, even off-shell, with same transverse space and same profiles for thebackground scalars. In this paper we restrict our discussion to tensorialfields only. In the context of bosonic string theory we consider on-shellpp-waves and argue that universality requires the existence of a universalsector of world-sheet operators whose correlation functions are insensitive tothe pp-wave nature of the metric and the background gauge flux. Such resultscan also be reproduced using the world-sheet conformal field theory. We alsostudy such pp-waves in non-polynomial closed string field theory (CSFT). Inparticular, we argue that for an off-shell pp-wave ansatz with flat transversespace and dilaton independent of transverse coordinates the field redefinitionrelating the low energy effective field theory and CSFT with all the massivemodes integrated out is at most quadratic in fields. Because of thissimplification it is expected that the off-shell pp-waves can be identified onthe two sides. Furthermore, given the massless pp-wave field configurations, aniterative method for computing the higher massive modes using the CSFTequations of motion has been discussed. All our bosonic string theory analysescan be generalised to the common Neveu-Schwarz sector of superstrings.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We report on the structural and magnetic properties of thin Ge(1-x)Mn(x)filmsgrown by molecular beam epitaxy (MBE) on Ge(001) substrates at temperatures(Tg) ranging from 80deg C to 200deg C, with average Mn contents between 1 % and11 %. Their crystalline structure, morphology and composition have beeninvestigated by transmission electron microscopy (TEM), electron energy lossspectroscopy and x-ray diffraction. In the whole range of growth temperaturesand Mn concentrations, we observed the formation of manganese richnanostructures embedded in a nearly pure germanium matrix. Growth temperaturemostly determines the structural properties of Mn-rich nanostructures. For lowgrowth temperatures (below 120deg C), we evidenced a two-dimensional spinodaldecomposition resulting in the formation of vertical one-dimensionalnanostructures (nanocolumns). Moreover we show in this paper the influence ofgrowth parameters (Tg and Mn content) on this decomposition i.e. on nanocolumnssize and density. For temperatures higher than 180deg C, we observed theformation of Ge3Mn5 clusters. For intermediate growth temperatures nanocolumnsand nanoclusters coexist. Combining high resolution TEM and superconductingquantum interference device magnetometry, we could evidence at least fourdifferent magnetic phases in Ge(1-x)Mn(x) films: (i) paramagnetic diluted Mnatoms in the germanium matrix, (ii) superparamagnetic and ferromagnetic low-Tcnanocolumns (120 K < Tc < 170 K), (iii) high-Tc nanocolumns (Tc> 400 K) and(iv) Ge3Mn5 clusters.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "By combining high-resolution (HST-WFPC2) and wide-field ground based (2.2mESO-WFI) and space (GALEX) observations, we have collected a multi-wavelengthphotometric data base (ranging from the far UV to the near infrared) of thegalactic globular cluster NGC1904 (M79). The sample covers the entire clusterextension, from the very central regions up to the tidal radius. In the presentpaper such a data set is used to study the BSS population and its radialdistribution. A total number of 39 bright ($m_{218}\\le 19.5$) BSS has beendetected, and they have been found to be highly segregated in the cluster core.No significant upturn in the BSS frequency has been observed in the outskirtsof NGC 1904, in contrast to other clusters (M 3, 47 Tuc, NGC 6752, M 5) studiedwith the same technique. Such evidences, coupled with the large radius ofavoidance estimated for NGC 1904 ($r_{avoid}\\sim 30$ core radii), indicate thatthe vast majority of the cluster heavy stars (binaries) has already sunk to thecore. Accordingly, extensive dynamical simulations suggest that BSS formed bymass transfer activity in primordial binaries evolving in isolation in thecluster outskirts represent only a negligible (0--10%) fraction of the overallpopulation.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "In this paper we demonstrate a technique of utilizing magnetically trappedneutral Rb-87 atoms to measure the magnitude and direction of stray electricfields emanating from surface contaminants. We apply an alternating externalelectric field that adds to (or subtracts from) the stray field in such a wayas to resonantly drive the trapped atoms into a mechanical dipole oscillation.The growth rate of the oscillation's amplitude provides information about themagnitude and sign of the stray field gradient. Using this measurementtechnique, we are able to reconstruct the vector electric field produced bysurface contaminants. In addition, we can accurately measure the electricfields generated from adsorbed atoms purposely placed onto the surface andaccount for their systematic effects, which can plague a precisionsurface-force measurement. We show that baking the substrate can reduce theelectric fields emanating from adsorbate, and that the mechanism for reductionis likely surface diffusion, not desorption.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We consider the problem of coloring the vertices of a large sparse randomgraph with a given number of colors so that no adjacent vertices have the samecolor. Using the cavity method, we present a detailed and systematic analyticalstudy of the space of proper colorings (solutions).  We show that for a fixed number of colors and as the average vertex degree(number of constraints) increases, the set of solutions undergoes several phasetransitions similar to those observed in the mean field theory of glasses.First, at the clustering transition, the entropically dominant part of thephase space decomposes into an exponential number of pure states so that beyondthis transition a uniform sampling of solutions becomes hard. Afterward, thespace of solutions condenses over a finite number of the largest states andconsequently the total entropy of solutions becomes smaller than the annealedone. Another transition takes place when in all the entropically dominantstates a finite fraction of nodes freezes so that each of these nodes isallowed a single color in all the solutions inside the state. Eventually, abovethe coloring threshold, no more solutions are available. We compute all thecritical connectivities for Erdos-Renyi and regular random graphs and determinetheir asymptotic values for large number of colors.  Finally, we discuss the algorithmic consequences of our findings. We arguethat the onset of computational hardness is not associated with the clusteringtransition and we suggest instead that the freezing transition might be therelevant phenomenon. We also discuss the performance of a simple local Walk-COLalgorithm and of the belief propagation algorithm in the light of our results.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present the results of a high-resolution X-ray imaging study of thestellar population in the Galactic massive star-forming region RCW49 and itscentral OB association Westerlund 2. We obtained a 40 ks X-ray image of a17'x17' field using the Chandra X-ray Observatory and deep NIR images using theInfrared Survey Facility in a concentric 8'3x8'3 region. We detected 468 X-raysources and identified optical, NIR, and Spitzer Space Telescope MIRcounterparts for 379 of them. The unprecedented spatial resolution andsensitivity of the X-ray image, enhanced by optical and infrared imaging data,yielded the following results: (1) The central OB association Westerlund 2 isresolved for the first time in the X-ray band. X-ray emission is detected fromall spectroscopically-identified early-type stars in this region. (2) Most(86%) X-ray sources with optical or infrared identifications are clustermembers in comparison with a control field in the Galactic Plane. (3) A looseconstraint (2--5 kpc) for the distance to RCW49 is derived from the mean X-rayluminosity of T Tauri stars. (4) The cluster X-ray population consists oflow-mass pre--main-sequence and early-type stars as obtained from X-ray and NIRphotometry. About 30 new OB star candidates are identified. (5) We estimate acluster radius of 6'--7' based on the X-ray surface number density profiles.(6) A large fraction (90%) of cluster members are identified individually usingcomplimentary X-ray and MIR excess emission. (7) The brightest five X-raysources, two Wolf-Rayet stars and three O stars, have hard thermal spectra.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "It is known that a macroscopic quantum superposition (MQS), when it isexposed to environment, decoheres at a rate scaling with the separation of itscomponent states in phase space. This is more or less consistent with the wellknown proposition that a more macroscopic quantum state is reduced more quicklyto a classical state in general. Effects of initial mixedness, however, on thesubsequent decoherence of MQSs have been less known. In this paper, we studythe evolution of a highly mixed MQS interacting with an environment, andcompare it with that of a pure MQS having the same size of the central distancebetween its component states. Although the decoherence develops more rapidlyfor the mixed MQS in short times, its rate can be significantly suppressedafter a certain time and becomes smaller than the decoherence rate of itscorresponding pure MQS. In an optics experiment to generate a MQS, our resulthas a practical implication that nonclassicality of a MQS can be stillobservable in moderate times even though a large amount of noise is added tothe initial state.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "In the conventional formulation of N=1 supersymmetry, a vector multiplet issupposed to be in the adjoint representation of a given gauge group. We presenta new formulation with a vector multiplet in the non-adjoint representation ofSO(N) gauge group. Our basic algebra is [ T^I, T^J ] = f^{I J K} T^K, [ T^I,U^i ] = - (T^I)^{i j} U^j, [ U^i, U^j ] = - (T^I)^{i j} T^I, where T^I are thegenerators of SO(N), while U^i are the new 'generators' in certain non-adjointreal representation R of SO(N). We use here the word `generator' in the broadersense of the word. Such a representation can be any real representation ofSO(N) with the positive definite metric, satisfying (T^I)^{i j} = - (T^I)^{j i}and (T^I)^{[ i j |} (T^I)^{| k ] l} \\equiv 0. The first non-trivial examplesare the spinorial 8_S and conjugate spinorial 8_C representations of SO(8)consistent with supersymmetry. We further couple the system to chiralmultiplets, and show that a Higgs mechanism can give positive definite (mass)^2to the new gauge fields for U^i. We show an analogous system working with N=1supersymmetry in 10D, and thereby N=4 system in 4D interacting with extramultiplets in the representation R. We also perform superspace reformulation asan independent confirmation.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Parton showers are widely used to generate fully exclusive final statesneeded to compare theoretical models to experimental observations. While, ingeneral, parton showers give a good description of the experimental data, theprecise functional form of the probability distribution underlying the eventgeneration is generally not known. The reason is that realistic parton showersare required to conserve four-momentum at each vertex. In this paper weinvestigate in detail how four-momentum conservation is enforced in a standardparton shower and why this destroys the analytic control of the probabilitydistribution. We show how to modify a parton shower algorithm such that itconserves four-momentum at each vertex, but for which the full analytic form ofthe probability distribution is known. We then comment how this analyticcontrol can be used to match matrix element calculations with parton showers,and to estimate effects of power corrections and other uncertainties in partonshowers.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The paper is considering an opportunity for the CERN/GranSasso (CNGS)neutrino complex, concurrent time-wise with T2K and NOvA, to search fortheta_13 oscillations and CP violation. Compared with large water Cherenkov(T2K) and fine grained scintillators (NOvA), the LAr-TPC offers a higherdetection efficiency and a lower backgrounds, since virtually all channels maybe unambiguously recognized. The present proposal, called MODULAr, describes a20 kt fiducial volume LAr-TPC, following very closely the technology developedfor the ICARUS-T60o, and is focused on the following activities, for which weseek an extended international collaboration:  (1) the neutrino beam from the CERN 400 GeV proton beam and an optimised hornfocussing, eventually with an increased intensity in the framework of the LHCaccelerator improvement program;  (2) A new experimental area LNGS-B, of at least 50000 m3 at 10 km off-axisfrom the main Laboratory, eventually upgradable to larger sizes. A location isunder consideration at about 1.2 km equivalent water depth;  (3) A new LAr Imaging detector of at least 20 kt fiducial mass. Such anincrease in the volume over the current ICARUS T600 needs to be carefullyconsidered. It is concluded that a very large mass is best realised with a setof many identical, independent units, each of 5 kt, \"cloning\" the technology ofthe T600. Further phases may foresee extensions of MODULAr to meet futurephysics goals.  The experiment might reasonably be operational in about 4/5 years, provided anew hall is excavated in the vicinity of the Gran Sasso Laboratory and adequatefunding and participation are made available.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "In this paper, we present a method to optimise rough set partition sizes, towhich rule extraction is performed on HIV data. The genetic algorithmoptimisation technique is used to determine the partition sizes of a rough setin order to maximise the rough sets prediction accuracy. The proposed method istested on a set of demographic properties of individuals obtained from theSouth African antenatal survey. Six demographic variables were used in theanalysis, these variables are; race, age of mother, education, gravidity,parity, and age of father, with the outcome or decision being either HIVpositive or negative. Rough set theory is chosen based on the fact that it iseasy to interpret the extracted rules. The prediction accuracy of equal widthbin partitioning is 57.7% while the accuracy achieved after optimising thepartitions is 72.8%. Several other methods have been used to analyse the HIVdata and their results are stated and compared to that of rough set theory(RST).", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The composite grain is made up of a host silicate spheroid and graphiteinclusions. The extinction efficiencies of the composite spheroidal grains forthree axial ratios are computed using the discrete dipole approximation (DDA).The interstellar extinction curve is evaluated in the spectral region3.40--0.10$\\mu m$ using the extinction efficiencies of the composite spheroidalgrains. The model extinction curves are then compared with the average observedinterstellar extinction curve. We also calculate the linear polarization forthe spheroidal composite grains at three orientation angles and find thewavelength of maximum polarization. Further, we estimate the volume extinctionfactor, an important parameter from the point of view of cosmic abundance, forthe composite grain models that reproduce the average observed interstellarextinction. The estimated abundances derived from the composite grain modelsfor both carbon and silicon are found to be lower than that are predicted bythe bare silicate/graphite grain models but these values are still higher thanthat are implied from the recent ISM values.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Classical and quantum phase transitions involve observables which arenon-analytic as functions of a controlled thermodynamical variable. As occurswith the self-consistent Fermi Golden Rule, one condition to obtain thediscontinuous behavior is the proper evaluation of a classical or quantumthermodynamic limit. We show that in presence of an environment, theoscillatory dynamics of a quantum two-level system, in analogy with a classicaldamped oscillator, can undergo a quantum dynamical phase transition to anon-oscillatory phase. This is obtained from a self-consistent solution of theGeneralized Landauer Buettiker Equations, a simplified integral form of theKeldysh formalism. I argue that working at each side of the transition impliesstanding under different paradigms in the Kuhn's sense of the word. Inconsequence, paradigms incommensurability obtains a sound mathematicaljustification as a consequence of the non-analyticity of the observables. Astrong case is made upon the need to deepen the public's intuition andunderstanding on the abrupt transition from static to dynamical frictionregimes.  Keywords: Self Consistent Fermi Golden Rule, Paradigm Shift, QuantumDynamical Phase Transition, Decoherence, Energy-time Wigner Function,Dissipative Two-level system, Keldysh Formalisma, GeneralizedLandauer-Buettiker Equations, Loschmidt Echo, Mesoscopic Echo, Spin Dynamics,Solid State NMR, Dynamical Quantum Zeno Effect, Liquid Crystal NMR.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Swift triggered on a precursor to the main burst of GRB 061121 (z=1.314),allowing observations to be made from the optical to gamma-ray bands. Manyother telescopes, including Konus-Wind, XMM-Newton, ROTSE and the FaulkesTelescope North, also observed the burst. The gamma-ray, X-ray and UV/opticalemission all showed a peak ~75s after the trigger, although the optical andX-ray afterglow components also appear early on - before, or during, the mainpeak. Spectral evolution was seen throughout the burst, with the promptemission showing a clear positive correlation between brightness and hardness.The Spectral Energy Distribution (SED) of the prompt emission, stretching from1eV up to 1MeV, is very flat, with a peak in the flux density at ~1keV. Theoptical-to-X-ray spectra at this time are better fitted by a broken, ratherthan single, power-law, similar to previous results for X-ray flares. The SEDshows spectral hardening as the afterglow evolves with time. This behaviourmight be a symptom of self-Comptonisation, although circumstellar densitiessimilar to those found in the cores of molecular clouds would be required. Theafterglow also decays too slowly to be accounted for by the standard models.Although the precursor and main emission show different spectral lags, both areconsistent with the lag-luminosity correlation for long bursts. GRB 061121 isthe instantaneously brightest long burst yet detected by Swift. Using acombination of Swift and Konus-Wind data, we estimate an isotropic energy of2.8x10^53 erg over 1keV - 10MeV in the GRB rest frame. A probable jet break isdetected at ~2x10^5s, leading to an estimate of ~10^51 erg for thebeaming-corrected gamma-ray energy.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "This paper presents the development of a new software in order to manageobjects, robots and mannequins in using the possibilities given by the hapticfeedback of the Phantom desktop devices. The haptic device provides 6positional degree of freedom sensing but three degrees force feedback. Thissoftware called eM-Virtual Desktop is integrated in the Tecnomatix's solutioncalled eM-Workplace. The eM-Workplace provides powerful solutions for planningand designing of complex assembly facilities, lines and workplaces. In thedigital mockup context, the haptic interfaces can be used to reduce thedevelopment cycle of products. Three different loops are used to manage thegraphic, the collision detection and the haptic feedback according to theirsown frequencies. The developed software is currently tested in industrialcontext by a European automotive constructor.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "In spectra of many Seyfert galaxies there is a wide emission line of Fe$K_\\alpha$. The line profile with two maxima supposes that the line emerges ininnermost regions of an accretion disk around a black hole, hence, it isnecessary to take into account General Relativity (GR) effects. In order todetermine GR processes which occur in active galactic nuclei (AGN) an inverseproblem of reconstructing the accreting system parameters from the line profilehas to be solved quickly. In this paper we present a numerical approximation ofthe emission line Fe $K_\\alpha$ with analytical functions. The approximation isaccomplished for a range of the disk radial coordinate $r$ and the angle$\\theta$ between line of sight and perpendicular to the disk and allows one todecrease computing time by $10^6$ times in certain astrophysical problemstaking into account all GR effects. The approximation results are available inthe Internet at http://www.iki.rssi.ru/people/repin/approx", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Effective Field Theory(EFT) is, the unique, model independent and systematiclow-energy version of QCD for processes involving momenta below the pion mass.A low-energy photo-nuclear observable in three-body systems, photonpolarization parameter at thermal neutron energies is calculated by usingpionless EFT up to next-to-next to leading order(N$^2$LO). In order to make acomparative study of this model, we compared our results for photonpolarization parameter with the realistic Argonne $v_{18}$ two-nucleon andUrbana IX or Tucson-Melbourne three-nucleon interactions. Three-body currentsgive small but significant contributions to some of the observables in theneutron-deuteron radiative capture cross section at thermal neutron energies.In this formalism the three-nucleon forces are needed up to N$^2$LO for cut-offindependent results. Our result converges order by order in low energyexpansion and also cut-off independent at this order.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "A game-theoretic framework is used to study the effect of constellation sizeon the energy efficiency of wireless networks for M-QAM modulation. Anon-cooperative game is proposed in which each user seeks to choose itstransmit power (and possibly transmit symbol rate) as well as the constellationsize in order to maximize its own utility while satisfying its delayquality-of-service (QoS) constraint. The utility function used here measuresthe number of reliable bits transmitted per joule of energy consumed, and isparticularly suitable for energy-constrained networks. The best-responsestrategies and Nash equilibrium solution for the proposed game are derived. Itis shown that in order to maximize its utility (in bits per joule), a user mustchoose the lowest constellation size that can accommodate the user's delayconstraint. Using this framework, the tradeoffs among energy efficiency, delay,throughput and constellation size are also studied and quantified. The effectof trellis-coded modulation on energy efficiency is also discussed.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The prediction of the three-dimensional native structure of proteins from theknowledge of their amino acid sequence, known as the protein folding problem,is one of the most important yet unsolved issues of modern science. Since theconformational behaviour of flexible molecules is nothing more than a complexphysical problem, increasingly more physicists are moving into the study ofprotein systems, bringing with them powerful mathematical and computationaltools, as well as the sharp intuition and deep images inherent to the physicsdiscipline. This work attempts to facilitate the first steps of such atransition. In order to achieve this goal, we provide an exhaustive account ofthe reasons underlying the protein folding problem enormous relevance andsummarize the present-day status of the methods aimed to solving it. We alsoprovide an introduction to the particular structure of these biologicalheteropolymers, and we physically define the problem stating the assumptionsbehind this (commonly implicit) definition. Finally, we review the 'specialflavor' of statistical mechanics that is typically used to study theastronomically large phase spaces of macromolecules. Throughout the whole work,much material that is found scattered in the literature has been put togetherhere to improve comprehension and to serve as a handy reference.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "If the recent PVLAS results on polarization changes of a linearly polarizedlaser beam passing through a magnetic field are interpreted by an axion-likeparticle, it is almost certain that it is not a standard QCD axion. Consideringthis, we study the general effective interactions of photons with spin-zeroparticles without restricting the latter to be a pseudo-scalar or a scalar,i.e., a parity eigenstate. At the lowest order in effective field theory, thereare two dimension-5 interactions, each of which has previously been treatedseparately for a pseudo-scalar or a scalar particle. By following the evolutionin an external magnetic field of the system of spin-zero particles and photons,we compute the changes in light polarization and the transition probability fortwo experimental set-ups: one-way propagation and round-trip propagation. Whilethe first may be relevant for astrophysical sources of spin-zero particles, thesecond applies to laboratory optical experiments like PVLAS. In the one-waypropagation, interesting phenomena can occur for special configurations ofpolarization where, for instance, transition occurs but light polarization doesnot change. For the round-trip propagation, however, the standard results ofpolarization changes for a pseudoscalar or a scalar are only modified by afactor that depends on the relative strength of the two interactions.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "It is proposed that radiation belts similar to the ones in the planetarymagnetosphere can exist for a pulsar with a relatively long period and a strongmagnetic field. In the belts located in the closed field line region near thelight cylinder relativistic pairs are trapped and maintained at a densitysubstantially higher than the local Goldreich-Julian corotation density. Thetrapped plasma can be supplied and replenished by either direct injection ofrelativistic pairs from acceleration of externally-supplied particles in adormant outer gap or in situ ionization of the accreted neutral material in thetrapping region. The radiation belts can be disrupted by waves that are excitedin the region as the result of plasma instabilities or emitted from the surfacedue to starquakes or stellar oscillations. The disruption can cause anintermittent particle precipitation toward the star producing radio bursts. Itis suggested that such bursts may be seen as rotating radio transients (RRATs).", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present the results of photoionization modeling of nine weak MgII (W_r<0.3Ang) quasar absorption line systems with redshifts 1.4<z<2.4 obtained with theUltraviolet and Visual Echelle Spectrograph on the Very Large Telescope. Thesesystems have been chosen because they provide access to a regime of red-shiftspace that previous weak MgII studies have not looked at. The densities,metallicities, Doppler parameters, and column densities of these systems arecompared to those of other weak MgII systems at lower redshift. There is nosignificant statistical variation in the properties of the absorbers over theredshift range 0.4<z<2.4. The number density per unit redshift is known todecrease for weak MgII absorbers between z~1 and z~2 by a greater amount thanpredicted from cosmological effects and changes in the extragalactic ionizingbackground alone. We suggest that, because the physical properties of theabsorber population are not seen to change significantly across this range,that the evolution in dN/dz is due to a decrease in the activity that givesrise to weak MgII absorption, and not due to a change in the processes thatform weak MgII absorbers. The presence of separate, but aligned (in velocity)low and high density clouds in all single cloud weak MgII absorbers provides animportant diagnostic of their geometry. We discuss possible origins in dwarfgalaxies and in extragalactic analogs to high velocity clouds.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We consider a two-brane system in a five-dimensional anti-de Sitterspacetime. We study particle creation due to the motion of the physical branewhich first approaches the second static brane (contraction) and then recedesfrom it(expansion). The spectrum and the energy density of the generatedgravitons are calculated. We show that the massless gravitons have a bluespectrum and that their energy density satisfies the nucleosynthesis bound withvery mild constraints on the parameters. We also show that the Kaluza-Kleinmodes cannot provide the dark matter in an anti-de-Sitter braneworld. However,for natural choices of parameters, backreaction from the Kaluza-Klein gravitonsmay well become important. The main findings of this work have been publishedin the form of a Letter [R. Durrer and M. Ruser, Phys. Rev. Lett. 99, 071601(2007), arXiv:0704.0756].", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We report the discovery of a substellar-mass companion to the K0-giant HD17092 with the Hobby-Eberly Telescope. In the absence of any correlation of theobserved 360-day periodicity with the standard indicators of stellar activity,the observed radial velocity variations are most plausibly explained in termsof a Keplerian motion of a planetary-mass body around the star. With theestimated stellar mass of 2.3Msun, the minimum mass of the planet is 4.6MJ. Theplanet's orbit is characterized by a mild eccentricity of e=0.17 and asemi-major axis of 1.3 AU. This is the tenth published detection of a planetarycompanion around a red giant star. Such discoveries add to our understanding ofplanet formation around intermediate-mass stars and they provide dynamicalinformation on the evolution of planetary systems around post-main sequencestars.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We calculate the thermal conductivity of electrons and muons kappa_{e-mu}produced owing to electromagnetic interactions of charged particles in neutronstar cores and show that these interactions are dominated by the exchange oftransverse plasmons (via the Landau damping of these plasmons innonsuperconducting matter and via a specific plasma screening in the presenceof proton superconductivity). For normal protons, the Landau damping stronglyreduces kappa_{e-mu} and makes it temperature independent. Protonsuperconductivity suppresses the reduction and restores the Fermi-liquidbehavior kappa_{e-mu} ~ 1/T. Comparing with the thermal conductivity ofneutrons kappa_n, we obtain kappa_{e-mu}> kappa_n for T>2 GK in normal matterand for any T in superconducting matter with proton critical temperaturesT_c>3e9 K. The results are described by simple analytic formulae.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "In this paper we obtain general integral formulas for probabilities in theasymmetric simple exclusion process (ASEP) on the integer lattice with nearestneighbor hopping rates p to the right and q=1-p to the left. For the most partwe consider an N-particle system but for certain of these formulas we can takethe limit as N goes to infinity. First we obtain, for the N-particle system, aformula for the probability of a configuration at time t, given the initialconfiguration. For this we use Bethe Ansatz ideas to solve the master equation,extending a result of Schuetz for the case N=2. The main results of the paper,derived from this, are integral formulas for the probability, for given initialconfiguration, that the m'th left-most particle is at x at time t. In one ofthese formulas we can take the limit as N goes to infinity, and it gives theprobability for an infinite system where the initial configuration is boundedon one side. For the special case of the totally asymmetric simple exclusionprocess (TASEP) our formulas reduce to the known ones.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "This paper investigates the many-to-one throughput capacity (and by symmetry,one-to-many throughput capacity) of IEEE 802.11 multi-hop networks. It hasgenerally been assumed in prior studies that the many-to-one throughputcapacity is upper-bounded by the link capacity L. Throughput capacity L is notachievable under 802.11. This paper introduces the notion of \"canonicalnetworks\", which is a class of regularly-structured networks whose capacitiescan be analyzed more easily than unstructured networks. We show that thethroughput capacity of canonical networks under 802.11 has an analytical upperbound of 3L/4 when the source nodes are two or more hops away from the sink;and simulated throughputs of 0.690L (0.740L) when the source nodes are manyhops away. We conjecture that 3L/4 is also the upper bound for generalnetworks. When all links have equal length, 2L/3 can be shown to be the upperbound for general networks. Our simulations show that 802.11 networks withrandom topologies operated with AODV routing can only achieve throughputs farbelow the upper bounds. Fortunately, by properly selecting routes near thegateway (or by properly positioning the relay nodes leading to the gateway) tofashion after the structure of canonical networks, the throughput can beimproved significantly by more than 150%. Indeed, in a dense network, it isworthwhile to deactivate some of the relay nodes near the sink judiciously.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We discuss the possibility to study oscillations of atmospheric neutrinos inthe ATLAS experiment at CERN. Due to the large total detector mass, asignificant number of events is expected, and during the shutdown phases of theLHC, reconstruction of these events will be possible with very good energy andangular resolutions, and with charge identification. We argue that 500 livedays of neutrino running could be achieved, and that a total of ~160 contained\\nu_\\mu events and ~360 upward going muons could be collected during this time.Despite the low statistics, the excellent detector resolution will allow for anunambiguous confirmation of atmospheric neutrino oscillations and formeasurements of the leading oscillation parameters. Though our detailedsimulations show that the sensitivity of ATLAS is worse than that of dedicatedneutrino experiments, we demonstrate that more sophisticated detectors, e.g. atthe ILC, could be highly competitive with upcoming superbeam experiments, andmight even give indications for the mass hierarchy and for the value oftheta-13.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Medvedev and Melott (2007) have suggested that periodicity in fossilbiodiversity may be induced by cosmic rays which vary as the Solar Systemoscillates normal to the galactic disk. We re-examine the evidence for a 62million year (Myr) periodicity in biodiversity throughout the Phanerozoichistory of animal life reported by Rohde & Mueller (2005), as well as relatedquestions of periodicity in origination and extinction. We find that the signalis robust against variations in methods of analysis, and is based onfluctuations in the Paleozoic and a substantial part of the Mesozoic.Examination of origination and extinction is somewhat ambiguous, with resultsdepending upon procedure. Origination and extinction intensity as defined by RMmay be affected by an artifact at 27 Myr in the duration of stratigraphicintervals. Nevertheless, when a procedure free of this artifact is implemented,the 27 Myr periodicity appears in origination, suggesting that the artifact mayultimately be based on a signal in the data. A 62 Myr feature appears inextinction, when this same procedure is used. We conclude that evidence for aperiodicity at 62 Myr is robust, and evidence for periodicity at approximately27 Myr is also present, albeit more ambiguous.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We investigate faint radio emission from low- to high-luminosity ActiveGalactic Nuclei (AGN) selected from the Sloan Digital Sky Survey (SDSS). Theirradio properties are inferred by co-adding large ensembles of radio imagecut-outs from the FIRST survey, as almost all of the sources are individuallyundetected. We correlate the median radio flux densities against a range ofother sample properties, including median values for redshift, [OIII]luminosity, emission line ratios, and the strength of the 4000A break. Wedetect a strong trend for sources that are actively undergoing star-formationto have excess radio emission beyond the ~10^28 ergs/s/Hz level found forsources without any discernible star-formation. Furthermore, this additionalradio emission correlates well with the strength of the 4000A break in theoptical spectrum, and may be used to assess the age of the star-formingcomponent. We examine two subsamples, one containing the systems with emissionline ratios most like star-forming systems, and one with the sources that havecharacteristic AGN ratios. This division also separates the mechanismresponsible for the radio emission (star-formation vs. AGN). For both cases wefind a strong, almost identical, correlation between [OIII] and radioluminosity, with the AGN sample extending toward lower, and the star-formationsample toward higher luminosities. A clearer separation between the twosubsamples is seen as function of the central velocity dispersion of the hostgalaxy. For systems with similar redshifts and velocity dispersions, thestar-formation subsample is brighter than the AGN in the radio by an order ofmagnitude. This underlines the notion that the radio emission in star-formingsystems can dominate the emission associated with the AGN.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We point out the evident errors in statistical analysis of the data,performed by Klapdor-Kleingrothaus et al in recently published paper toestablish a limit on the stability of electron with respect to the decay into$\\nu+\\gamma$. We performed the reestimation of the sensitivity of theexperimental setups to the 256 keV gamma emitted in the hypothetical electrondecay, and show that in [1] the limits on the electron stability and chargenonconservation parameter $\\epsilon_{e\\nu\\gamma}^{2}$ are overestimated by atleast a factor of 5. We have revealed evident errors in the statisticalanalysis, performed by Klapdor-Kleingrothaus et al in a recently publishedpaper [1] to establish a limit on the stability of electron with respect to thedecay into $\\nu+\\gamma$. The performed reestimation of the sensitivity of theexperimental setups to the 256 keV gamma emitted in the hypothetical electrondecay, has shown that the limits on the electron stability and chargenonconservation parameter $\\epsilon_{e\\nu\\gamma}^{2}$ presented in [1], havebeen overestimated by at least a factor of 5.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Cooperative diversity systems are wireless communication systems designed toexploit cooperation among users to mitigate the effects of multipath fading. Infairly general conditions, it has been shown that these systems can achieve thediversity order of an equivalent MISO channel and, if the node geometrypermits, virtually the same outage probability can be achieved as that of theequivalent MISO channel for a wide range of applicable SNR. However, much ofthe prior analysis has been performed under the assumption of perfect timingand frequency offset synchronization. In this paper, we derive the estimationbounds and associated maximum likelihood estimators for frequency offsetestimation in a cooperative communication system. We show the benefit ofadaptively tuning the frequency of the relay node in order to reduce estimationerror at the destination. We also derive an efficient estimation algorithm,based on the correlation sequence of the data, which has mean squared errorclose to the Cramer-Rao Bound.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present an atlas of the central regions of 75 Seyfert galaxies imaged inthe near-UV with the Advanced Camera for Surveys of the Hubble Space Telescopeat an average resolution of ~10pc. These data complement archival highresolution data from the Space Telescope at optical and near-IR wavelengths,creating an extremely valuable dataset for astronomers with a broad range ofscientific interests. Our goal is to investigate the nature of the near-UVlight in these objects, its relation to the circumnuclear starburst phenomenon,and the connection of this to the evolution and growth of the galaxy bulge andcentral black hole. In this paper, we describe the near-UV morphology of theobjects and characterize the near-UV emission. We estimate the size and theluminosity of the emitting regions and extract the luminosity profile. We alsodetermine the presence of unresolved compact nuclei. In addition, thecircumnuclear stellar cluster population is identified, and the contribution ofthe stellar clusters to the total light, at this wavelength, is estimated. Thesize of the sample allows us to draw robust statistical conclusions. We findthat {Seyfert 1} galaxies are completely dominated by its bright and compactnucleus, that remains point-like at this resolution, while we find almost nounresolved nucleus in Seyfert 2. The Seyfert types 1 and 2 are quite segregatedin an asymmetry vs compactness plot. Stellar clusters are found somewhat morefrequently in Sy2 (in ~70% of the galaxies) than in Sy1 (~57%), and contributemore to the total light in Sy2, but this two differences seem to be mostly dueto the large contribution of the compact nucleus in Sy1, as the luminositydistribution of the clusters is similar in both Sy types.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The effect of fractal normal-phase clusters on vortex dynamics in apercolative superconductor is considered. The superconductor containspercolative superconducting cluster carrying a transport current and clustersof a normal phase, acting as pinning centers. A prototype of such a structureis YBCO film, containing clusters of columnar defects, as well as the BSCCO/Agsheathed tape, which is of practical interest for wire fabrication. Transitionof the superconductor into a resistive state corresponds to the percolationtransition from a pinned vortex state to a resistive state when the vorticesare free to move. The dependencies of the free vortex density on the fractaldimension of the cluster boundary as well as the resistance on the transportcurrent are obtained. It is revealed that a mixed state of the vortex glasstype is realized in the superconducting system involved. The current-voltagecharacteristics of superconductors containing fractal clusters are obtained andtheir features are studied.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Several years ago, we proposed a modification of the Standard Model, in whichthe Higgs sector was stabilized by the addition of higher derivative operators,similar to Lee-Wick Electrodynamics. We studied this theory extensively, bothusing continuum Hamiltonian and path integral methods. We also reporteddetailed lattice studies of the higher derivative Higgs sector. In view of somerecent revived interest in our original idea, we are providing here ourextensive notes from the time period on this topic. The key results werealready published in our papers at that time. The many additional details thatwe make available here were previously available only in Chuan Liu's UCSD Ph.D.thesis (1994). Very recently, our idea has been revived by other groups. Inview of the renewed interest, and to perhaps correct some misconceptions in theliterature, we are here making our original extensive notes available to thewider community.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The composition of the eta and eta' mesons has long been a source ofdiscussion and is of current interest with new experimental results appearing.We investigate what can be learnt from a number of different processes: V to Pgamma and P to V gamma (V and P are light vector and pseudoscalar mesonsrespectively), P to gamma gamma, J/psi,psi' to P gamma, J/psi,psi' to P V, andchi_{c0,2} to PP. These constrain the eta-eta' mixing angle to a consistentvalue, phi approx 42 degrees; we find that the c cbar components are lesssim 5%in amplitude. We also find that, while the data hint at a small gluoniccomponent in the eta', the conclusions depend sensitively on unknown formfactors associated with exclusive dynamics. In addition, we predict BR(psi' toeta' gamma) approx 1 10^{-5} and BR(chi_{c0} to eta eta') approx 2 10^{-5} - 110^{-4}. We provide a method to test the mixing using chi_{c2} to eta eta, eta'eta', and eta eta' modes and make some general observations on chi_{c0,2}decays. We also survey the semileptonic and hadronic decays of bottom andcharmed mesons and find some modes where the mixing angle can be extractedcleanly with the current experimental data, some where more data will allowthis, and some where a more detailed knowledge of the different amplitudes isrequired.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Although powers of the Young-Jucys-Murphya elements X_i = (1 i) + ... +(i-1i), i = 1, ..., n, in the symmetric group S_n acting on {1, ...,n} do not liein the centre of the group algebra of S_n, we show that transitive powers,namely the sum of the contributions from elements that act transitively on {1,>...,n}, are central. We determine the coefficients, which we call starfactorization numbers, that occur in the resolution of transitive powers withrespect to the class basis of the centre of S_n, and show that they have apolynomiality property. These centrality and polynomiality properties haveseemingly unrelated consequences. First, they answer a question raised by Pakabout reduced decompositions; second, they explain and extend the beautifulsymmetry result discovered by Irving and Rattan; and thirdly, we relate thepolynomiality to an existing polynomiality result for a class of double Hurwitznumbers associated with branched covers of the sphere, which therefore suggeststhat there may be an ELSV-type formula associated with the star factorizationnumbers.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "In this paper we introduce a variant of pushdown dimension called boundedpushdown (BPD) dimension, that measures the density of information contained ina sequence, relative to a BPD automata, i.e. a finite state machine equippedwith an extra infinite memory stack, with the additional requirement that everyinput symbol only allows a bounded number of stack movements. BPD automata area natural real-time restriction of pushdown automata. We show that BPDdimension is a robust notion by giving an equivalent characterization of BPDdimension in terms of BPD compressors. We then study the relationships betweenBPD compression, and the standard Lempel-Ziv (LZ) compression algorithm, andshow that in contrast to the finite-state compressor case, LZ is not universalfor bounded pushdown compressors in a strong sense: we construct a sequencethat LZ fails to compress signicantly, but that is compressed by at least afactor 2 by a BPD compressor. As a corollary we obtain a strong separationbetween finite-state and BPD dimension.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We consider position measurements using the cross-correlated output of twotunnel junction position detectors. Using a fully quantum treatment, wecalculate the equation of motion for the density matrix of the coupleddetector-detector-mechanical oscillator system. After discussing the presenceof a bound on the peak-to-background ratio in a position measurement using asingle detector, we show how one can use detector cross correlations toovercome this bound. We analyze two different possible experimentalrealizations of the cross correlation measurement and show that in both casesthe maximum cross-correlated output is obtained when using twin detectors andapplying equal bias to each tunnel junction. Furthermore, we show how thedouble-detector setup can be exploited to drastically reduce the addeddisplacement noise of the oscillator.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The common wisdom that the phonon mechanism of electron pairing in theweak-coupling Bardeen-Cooper-Schrieffer (BCS) superconductors leads toconventional s-wave Cooper pairs is revised. An inevitable anisotropy of soundvelocity in crystals makes the phonon-mediated attraction of electronsnon-local in space providing unconventional Cooper pairs with a nonzero orbitalmomentum in a wide range of electron densities. As a result of this anisotropyquasi-two dimensional charge carriers undergo a quantum phase transition froman unconventional d-wave superconducting state to a conventional s-wavesuperconductor with more carriers per unit cell. In the oppositestrong-coupling regime rotational symmetry breaking appears as a result of areduced Coulomb repulsion between unconventional bipolarons dismissing therebysome constraints on unconventional pairing in the Bose-Einstein condensation(BEC) limit. The conventional phonons, and not superexchange, are shown to beresponsible for the d-wave symmetry of cuprate superconductors, where theon-site Coulomb repulsion is large.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "It has been claimed that the observed magnitude of the vacuum energy densityis consistent with the distribution predicted in anthropic models, in which anensemble of universes is assumed. This calculation is revisited, without makingthe assumption that the CMB temperature is known, and considering in detail thepossibility of a recollapsing universe. New accurate approximations for thegrowth of perturbations and the mass function of dark haloes are presented.Structure forms readily in the recollapsing phase of a model with negativeLambda, so collapse fraction alone cannot forbid Lambda from being large andnegative. A negative Lambda is disfavoured only if we assume that formation ofobservers can be neglected once the recollapsing universe has heated to T > 8K. For the case of positive Lambda, however, the current universe does occupy aextremely typical position compared to the predicted distribution on theLambda-T plane. Contrasting conclusions can be reached if anthropic argumentsare applied to the curvature of the universe, and we discuss the falsifiabilityof this mode of anthropic reasoning.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We have used the Very Large Array (VLA) to search for radio emission from theglobular cluster G1 (Mayall-II) in M31. G1 has been reported by Gebhardt et al.to contain an intermediate-mass black hole (IMBH) with a mass of ~2 x 10^4solar masses. Radio emission was detected within an arcsecond of the clustercenter with an 8.4 GHz power of 2 x 10^{15} W/Hz. The radio/X-ray ratio of G1is a few hundred times higher than that expected for a high-mass X-ray binaryin the cluster center, but is consistent with the expected value for accretiononto an IMBH with the reported mass. A pulsar wind nebula is also a possiblecandidate for the radio and X-ray emission from G1; future high-sensitivityVLBI observations might distinguish between this possibility and an IMBH. Ifthe radio source is an IMBH, and similar accretion and outflow processes occurfor hypothesized ~ 1000-solar-mass black holes in Milky Way globular clusters,they are within reach of the current VLA and should be detectable easily by theExpanded VLA when it comes on line in 2010.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We revisit the model of a system made up of a Brownian quantum oscillatorunder the influence of an external classical force and linearly coupled to anenvironment made up of many quantum oscillators at zero or finite temperature.We show that the HPZ master equation for the reduced density matrix derivedearlier [B.L. Hu, J.P. Paz, Y. Zhang, Phys. Rev. D 45, 2843 (1992)] withcoefficients obtained from solutions of integro-differential equations canassume closed functional forms for a fairly general class of spectral densitiesof the environment at arbitrary temperature and coupling strength. As anillustration of these new results we solve the corresponding master equationand calculate, among other physical quantities, the uncertainty function whoselate time behavior can be obtained fully. This produces a formula forinvestigating the standard quantum limit which is central to addressing manytheoretical issues in macroscopic quantum phenomena and experimental concernsrelated to low temperature precision measurements. We find that any initialstate always settles down to a Gaussian density matrix whose covariance isdetermined by the thermal reservoir and whose mean is determined by theexternal force. For more general spectra we show that the solution of themaster equation can be reduced to solving for the motion of a classicalparametric oscillator with parametric frequency determined by the unsolved formaster equation coefficients. States in these systems experience evolution thatis parametrically similar to the simpler evolution explicitly determined for inthe case of Laurent-series spectra.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present a theoretical study of the interplay between cyclotron motion andspin splitting of charge carriers in solids. While many of our results applymore generally, we focus especially on discussing the Rashba model describingelectrons in the conduction band of asymmetric semiconductor heterostructures.Appropriate semiclassical limits are distinguished that describe varioussituations of experimental interest. Our analytical fomulae, which take fullaccount of Zeeman splitting, are used to analyse recent magnetic-focusing data.Surprisingly, it turns out that the Rashba effect can dominate the splitting ofcyclotron orbits even when the Rashba and Zeeman spin-splitting energies are ofthe same order. We also find that the origin of spin-dependent cyclotron motioncan be traced back to Zitterbewegung-like oscillatory dynamics of chargecarriers from spin-split bands. The relation between the two phenomena isdiscussed, and we estimate the effect of Zitterbewegung-related corrections tothe charge carriers' canonical position.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The transition between the low density groups of T Tauri stars and the highdensity clusters around massive stars occurs in the intermediate-mass (IM)range (M$_*$$\\sim$2--8 M$_\\odot$). High spatial resolution studies of IM youngstellar objects (YSO) can provide important clues to understand the clusteringin massive star forming regions.  Aims: Our aim is to search for clustering in IM Class 0 protostars. The highspatial resolution and sensitivity provided by the new A configuration of thePlateau de Bure Interferometer (PdBI) allow us to study the clustering in thesenearby objects.  Methods: We have imaged three IM Class 0 protostars (Serpens-FIRS 1, IC 1396N, CB 3) in the continuum at 3.3 and 1.3mm using the PdBI. The sources havebeen selected with different luminosity to investigate the dependence of theclustering process on the luminosity of the source.  Results: Only one millimeter (mm) source is detected towards the lowluminosity source Serpens--FIRS 1. Towards CB 3 and IC1396 N, we detect twocompact sources separated by $\\sim$0.05 pc. The 1.3mm image of IC 1396 N, whichprovides the highest spatial resolution, reveal that one of these cores issplitted in, at least, three individual sources.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The topological insulator is an electronic phase stabilized by spin-orbitcoupling that supports propagating edge states and is not adiabaticallyconnected to the ordinary insulator. In several ways it is a spin-orbit-inducedanalogue in time-reversal-invariant systems of the integer quantum Hall effect(IQHE). This paper studies the topological insulator phase in disorderedtwo-dimensional systems, using a model graphene Hamiltonian introduced by Kaneand Mele as an example. The nonperturbative definition of a topologicalinsulator given here is distinct from previous efforts in that it involvesboundary phase twists that couple only to charge, does not refer to edgestates, and can be measured by pumping cycles of ordinary charge. In thisdefinition, the phase of a Slater determinant of electronic states isdetermined by a Chern parity analogous to Chern number in the IQHE case.Numerically we find, in agreement with recent network model studies, that thedirect transition between ordinary and topological insulators that occurs inband structures is a consequence of the perfect crystalline lattice.Generically these two phases are separated by a metallic phase, which isallowed in two dimensions when spin-orbit coupling is present. The sameapproach can be used to study three-dimensional topological insulators.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The groups G_{k,1} of Richard Thompson and Graham Higman can be generalizedin a natural way to monoids, that we call M_{k,1}, and to inverse monoids,called Inv_{k,1}; this is done by simply generalizing bijections to partialfunctions or partial injective functions. The monoids M_{k,1} have connectionswith circuit complexity (studied in another paper). Here we prove that M_{k,1}and Inv_{k,1} are congruence-simple for all k. Their Green relations J and Dare characterized: M_{k,1} and Inv_{k,1} are J-0-simple, and they have k-1non-zero D-classes. They are submonoids of the multiplicative part of the Cuntzalgebra O_k. They are finitely generated, and their word problem over anyfinite generating set is in P. Their word problem is coNP-complete over certaininfinite generating sets.  Changes in this version: Section 4 has been thoroughly revised, and errorshave been corrected; however, the main results of Section 4 do not change.Sections 1, 2, and 3 are unchanged, except for the proof of Theorem 2.3, whichwas incomplete; a complete proof was published in the Appendix of reference[6], and is also given here.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Community structure is an important property of complex networks. Anautomatic discovery of such structure is a fundamental task in manydisciplines, including sociology, biology, engineering, and computer science.Recently, several community discovery algorithms have been proposed based onthe optimization of a quantity called modularity (Q). However, the problem ofmodularity optimization is NP-hard, and the existing approaches often sufferfrom prohibitively long running time or poor quality. Furthermore, it has beenrecently pointed out that algorithms based on optimizing Q will have aresolution limit, i.e., communities below a certain scale may not be detected.In this research, we first propose an efficient heuristic algorithm, Qcut,which combines spectral graph partitioning and local search to optimize Q.Using both synthetic and real networks, we show that Qcut can find highermodularities and is more scalable than the existing algorithms. Furthermore,using Qcut as an essential component, we propose a recursive algorithm, HQcut,to solve the resolution limit problem. We show that HQcut can successfullydetect communities at a much finer scale and with a higher accuracy than theexisting algorithms. Finally, we apply Qcut and HQcut to study aprotein-protein interaction network, and show that the combination of the twoalgorithms can reveal interesting biological results that may be otherwiseundetectable.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The description of the statistical properties of dust emission givesimportant constraints on the physics of the interstellar medium but it is alsoa useful way to estimate the contamination of diffuse interstellar emission inthe cases where it is considered a nuisance. The main goals of this analysis ofthe power spectrum and non-Gaussian properties of 100 micron dust emission are1) to estimate the power spectrum of interstellar matter density in threedimensions, 2) to review and extend previous estimates of the cirrus noise dueto dust emission and 3) to produce simulated dust emission maps that reproducethe observed statistical properties. The main results are the following. 1) Thecirrus noise level as a function of brightness has been previouslyoverestimated. It is found to be proportional to <I> instead of <I>^1.5, where<I> is the local average brightness at 100 micron. This scaling is inaccordance with the fact that the brightness fluctuation level observed at agiven angular scale on the sky is the sum of fluctuations of increasingamplitude with distance on the line of sight. 2) The spectral index of dustemission at scales between 5 arcmin and 12.5 degrees is <gamma>=-2.9 on averagebut shows significant variations over the sky. Bright regions havesystematically steeper power spectra than diffuse regions. 3) The skewness andkurtosis of brightness fluctuations is high, indicative of strongnon-Gaussianity. 4) Based on our characterization of the 100 micron powerspectrum we provide a prescription of the cirrus confusion noise as a functionof wavelength and scale. 5) Finally we present a method based on a modificationof Gaussian random fields to produce simulations of dust maps which reproducethe power spectrum and non-Gaussian properties of interstellar dust emission.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We have investigated a closed system of equations for the quark propagator,obtained earlier within our general approach to QCD at low energies. It impliesquark confinement (the quark propagator has no pole, indeed), as well as thedynamical breakdown of chiral symmetry (a chiral symmetry preserving solutionis forbidded). This system can be solved exactly in the chiral limit. We haveestablished the space of the smooth test functions (consisting of the Green'sfunctions for the quark propagator and the corresponding quark-gluon vertex) inwhich our generalized function (the confining gluon propagator) becomes acontinuous linear functional. It is a linear topological space $K(c)$ of theinfinitely differentiable functions (with respect to the dimensionless momentumvariable $x$), having compact support in the region $x \\leq c$. We develop ananalytical formalism, the so-called chiral perturbtion theory at thefundamental quark level, which allows one to find explicit solution for thequark propagator in powers of the light quark masses. We also develop ananalytical formalism, which allows one to find the solution for the quarkpropagator in the inverse powers of the heavy quark masses. It justifies theuse for the heavy quark propagator its free counterpart up to terms of theorder $1/m_Q^3$, where $m_Q$ is the heavy quark mass. So this solutionautomatically possesses the heavy quark spin-flavor symmetry.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "In this paper we consider module-composed graphs, i.e. graphs which can bedefined by a sequence of one-vertex insertions v_1,...,v_n, such that theneighbourhood of vertex v_i, 2<= i<= n, forms a module (a homogeneous set) ofthe graph defined by vertices v_1,..., v_{i-1}.  We show that module-composed graphs are HHDS-free and thus homogeneouslyorderable, weakly chordal, and perfect. Every bipartite distance hereditarygraph, every (co-2C_4,P_4)-free graph and thus every trivially perfect graph ismodule-composed. We give an O(|V_G|(|V_G|+|E_G|)) time algorithm to decidewhether a given graph G is module-composed and construct a correspondingmodule-sequence.  For the case of bipartite graphs, module-composed graphs are exactly distancehereditary graphs, which implies simple linear time algorithms for theirrecognition and construction of a corresponding module-sequence.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "In many applications, input data are sampled functions taking their values ininfinite dimensional spaces rather than standard vectors. This fact has complexconsequences on data analysis algorithms that motivate modifications of them.In fact most of the traditional data analysis tools for regression,classification and clustering have been adapted to functional inputs under thegeneral name of functional Data Analysis (FDA). In this paper, we investigatethe use of Support Vector Machines (SVMs) for functional data analysis and wefocus on the problem of curves discrimination. SVMs are large margin classifiertools based on implicit non linear mappings of the considered data into highdimensional spaces thanks to kernels. We show how to define simple kernels thattake into account the unctional nature of the data and lead to consistentclassification. Experiments conducted on real world data emphasize the benefitof taking into account some functional aspects of the problems.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We discuss how, in a Universe restricted to the causal region connected tothe observer, General Relativity implies the quantum nature of physicalphenomena and directly leads to a string theory scenario, whose dynamics isruled by a functional that weights all configurations according to theirentropy. The most favoured configurations are those of minimal entropy. Alongthis class of vacua a four-dimensional space-time is automatically selected;when, at large volume, a description of space-time in terms of classicalgeometry can be recovered, the entropy-weighted sum reduces to the ordinaryFeynman's path integral. What arises is a highly predictive scenario,phenomenologically compatible with the experimental observations andmeasurements, in which everything is determined in terms of the fundamentalconstants and the age of the Universe, with no room for freely-adjustableparameters. We discuss how this leads to the known spectrum of particles andinteractions. Besides the computation of masses and couplings, CKM matrixelements, cosmological constant, expansion parameters of the Universe etc...,all resulting, within the degree of the approximation we used, in agreementwith the experimental observations, we also discuss how this scenario passesthe tests provided by cosmology and the constraints imposed by the physics ofthe primordial Universe.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We have presented a detailed study of twist-2 and twist-3 light-conedistribution amplitudes of $1^3P_1$ and $1^1P_1$ axial-vector mesons, based onQCD conformal partial wave expansion. Applying equations of motion, thetwist-three two-parton light-cone distribution amplitudes can be expressed interms of leading-twist and twist-three three-parton light-cone distributionamplitudes. The relevant G-parity invariant and violating parameters,containing the corrections due to the SU(3) breaking effects, are evaluatedfrom the QCD sum rule method. The results for axial-vector decay constants of$1^3P_1$ states are presented. The values of tensor decay constants andGegenbauer moments of the leading twist distribution amplitudes for $1^1P_1$states are updated. Using Gell-Mann-Okubo mass formula, the mixing angle forthe $f_8$ and $f_1$ of $1^3P_1$ states is $\\theta_{^3P_1}\\sim 38^\\circ$, andthat for $h_8$ and $h_1$ of $1^1P_1$ states is $\\theta_{^1P_1}\\sim 10^\\circ$.The detailed properties for physical states $f_1(1285), f_1(1420), h_1(1170)$,and $h_1(1380)$ are given. Assuming the mixing angle between $K_{1A}$ and$K_{1B}$ to be $\\theta_K=45^\\circ$ or $-45^\\circ$, we also give the detailedstudy for $K_1(1270)$ and $K_1(1400)$. Using the conformal partial waveexpansion, we obtain the models for light-cone distribution amplitudes,containing contributions up to conformal spin 9/2. It is interesting to notethat some distribution amplitudes have significant asymmetric behaviors, whichshould be phenomenologically attractive.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Context. Although Blazars are a small fraction of the overall AGN populationthey are expected to be the dominant population of extragalactic sources in thehard X-ray and gamma-ray bands and have been shown to be the largestcontaminant of CMB fluctuation maps. So far the number of known blazars is ofthe order of several hundreds, but the forthcoming AGILE, GLAST and Planckspace observatories will detect several thousand of objects of this type. Aims.In preparation for these missions it is necessary to identify new samples ofblazars to study their multi-frequency characteristics and statisticalproperties. Methods. We compiled a sample of objects with blazar-likeproperties via a cross-correlation between large radio (NVSS, ATCAPMN) and X-ray surveys (RASS) using the SDSS-DR4 and 2dF survey data to spectroscopicallyidentify our candidates and test the validity of the selection method. Results.We present the Radio - Optical - X-ray catalog built at ASDC (ROXA), a list of816 objects among which 510 are confirmed blazars. Only 19% of the candidatesturned out to be certainly non-blazars demonstrating the high efficiency of ourselection method. Conclusions. Our catalog includes 173 new blazaridentifications, or about 10% of all presently known blazars. The relativelyhigh flux threshold in the X-ray energy band (given by the RASS survey)preferentially selects objects with high fx / fr ratio leading to the discoveryof new High Energy Peaked BL Lac (HBLs). Our catalog therefore includes manynew potential targets for GeV-TeV observations.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "If predictions for species extinctions hold, then the `tree of life' todaymay be quite different to that in (say) 100 years. We describe a technique toquantify how much each species is likely to contribute to future biodiversity,as measured by its expected contribution to phylogenetic diversity. Ourapproach considers all possible scenarios for the set of species that will beextant at some future time, and weights them according to their likelihoodunder an independent (but not identical) distribution on species extinctions.Although the number of extinction scenarios can typically be very large, weshow that there is a simple algorithm that will quickly compute this index. Themethod is implemented and applied to the prosimian primates as a test case, andthe associated species ranking is compared to a related measure (the `Shapleyindex'). We describe indices for rooted and unrooted trees, and a modificationthat also includes the focal taxon's probability of extinction, making itdirectly comparable to some new conservation metrics.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "In the past both instrumentalism and empiricism have inspired certainpragmatic elements into the Copenhagen interpretation of quantum mechanics. Therelation of such pragmatisms with the correspondence principle is discussed. Itis argued that neither Bohr nor Heisenberg did take `correspondence' in one ofthese forms, and that it, in particular, was Bohr's classical attitude whichcaused him to apply in an inconsistent way his correspondence principle to theEinstein-Podolsky-Rosen experiment, thus causing much confusion. It isdemonstrated that an empiricist pragmatism is conducive to an explanation ofviolation of the Bell inequalities as a consequence of `complementarity' in thesense of `mutual disturbance in a joint nonideal measurement of incompatibleobservables' rather than as being caused by `nonlocal influences'.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We investigate the possibility of a dark energy universe emerging from anaction with higher-order string loop corrections to Einstein gravity in thepresence of a massless dilaton. These curvature corrections (up to $R^4$ order)are different depending upon the type of (super)string model which isconsidered. We find in fact that Type II, heterotic, and bosonic stringsrespond differently to dark energy. A dark energy solution is shown to exist inthe case of the bosonic string, while the other two theories do not lead torealistic dark energy universes. Detailed analysis of the dynamical stabilityof the de-Sitter solution is presented for the case of a bosonic string. Ageneral prescription for the construction of a de-Sitter solution for thelow-energy (super)string effective action is also indicated. Beyond thelow-energy (super)string effective action, when the higher-curvature correctioncoefficients depend on the dilaton, the reconstruction of the theory from theuniverse expansion history is done with a corresponding prescription for thescalar potentials.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "To improve the quality of life in a modern society it is essential to reducethe distance between basic research and applications, whose crucial roles inshaping today's society prompt us to seek their understanding. Existing studieson this subject, however, have neglected the network character of theinteraction between university and industry. Here we use state-of-the-artnetwork theory methods to analyze this interplay in the so-called FrameworkProgramme--an initiative which sets out the priorities for the European Union'sresearch and technological development. In particular we study in the 5thFramework Programme (FP5) the role played by companies and scientificinstitutions and how they contribute to enhance the relationship betweenresearch and industry. Our approach provides quantitative evidence that whilefirms are size hierarchically organized, universities and researchorganizations keep the network from falling into pieces, paving the way for aneffective knowledge transfer.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "It is known that a subset of fractional quantum Hall wave functions has beenexpressed as conformal field theory (CFT) correlators, notably the Laughlinwave function at filling factor $\\nu=1/m$ ($m$ odd) and its quasiholes, and thePfaffian wave function at $\\nu=1/2$ and its quasiholes. We develop a generalscheme for constructing composite-fermion (CF) wave functions from conformalfield theory. Quasiparticles at $\\nu=1/m$ are created by inserting anyonicvertex operators, $P_{\\frac{1}{m}}(z)$, that replace a subset of the electronoperators in the correlator. The one-quasiparticle wave function is identicalto the corresponding CF wave function, and the two-quasiparticle wave functionhas correct fractional charge and statistics and is numerically almostidentical to the corresponding CF wave function. We further show how to exactlyrepresent the CF wavefunctions in the Jain series $\\nu = s/(2sp+1)$ as the CFTcorrelators of a new type of fermionic vertex operators, $V_{p,n}(z)$,constructed from $n$ free compactified bosons; these operators provide the CFTrepresentation of composite fermions carrying $2p$ flux quanta in the $n^{\\rmth}$ CF Landau level. We also construct the corresponding quasiparticle- andquasihole operators and argue that they have the expected fractional charge andstatistics. For filling fractions 2/5 and 3/7 we show that the chiral CFTs thatdescribe the bulk wave functions are identical to those given by Wen's generalclassification of quantum Hall states in terms of $K$-matrices and $l$- and$t$-vectors, and we propose that to be generally true. Our results suggest ageneral procedure for constructing quasiparticle wave functions for otherfractional Hall states, as well as for constructing ground states at fillingfractions not contained in the principal Jain series.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present a theoretical study of the density of states and supercurrent indiffusive superconductor-normal metal-superconductor (SNS) junctions. Inparticular, we study the influence on these two equilibrium properties of bothan arbitrary transparency of the SN interfaces and the presence of spin-flipscattering in the normal wire. We show that the minigap that is present in thespectrum of the diffusive wire is very sensitive to the interface transmission.More mportantly, we show that at arbitrary transparency the minigap replacesthe Thouless energy as the relevant energy scale for the proximity effect,determining for instance the temperature dependence of the critical current. Wealso study in detail how the critical current is suppressed by the effect ofspin-flip scattering, which can be due to either magnetic impurities or, undercertain circumstances, to an external magnetic field. Our analysis based on thequasiclassical theory of diffusive superconductors can be very valuable toestablish quantitative comparisons between experiment and theory.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Phonon transmission across epitaxial interfaces is studied within the latticedynamic approach. The transmission shows weak dependence on frequency for thelattice wave with a fixed angle of incidence. The dependence on azimuth angleis found to be related to the symmetry of the boundary interface. Thetransmission varies smoothly with the change of the incident angle. A criticalangle of incidence exists when the phonon is incident from the side with largegroup velocities to the side with low ones. No significant mode conversion isobserved among different acoustic wave branches at the interface, except whenthe incident angle is near the critical value. Our theoretical result of theKapitza conductance $G_{K}$ across the Si-Ge (100) interface at temperature$T=200 $K is $4.6\\times10^{8} {\\rm WK}^{-1}{\\rmm}^{-2}$. A scaling law $G_K\\propto T^{2.87}$ at low temperature is also reported. Based on the features oftransmission obtained within lattice dynamic approach, we propose a simplifiedformula for thermal conductanceacross the epitaxial interface. A reasonableconsistency is found between the calculated values and the experimentallymeasured ones.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present a new, deep (V ~ 26) study of the Galactic globular cluster NGC2419 based on B,V,I time-series CCD photometry over about 10 years andextending beyond the cluster published tidal radius. We have identified 101variable stars of which 60 are new discoveries, doubling the known RR Lyraestars and including 12 SX Phoenicis stars. The average period of the RR Lyraestars (<Pab>=0.662 d, and <Pc>=0.366 d, for fundamental-mode -RRab- andfirst-overtone pulsators, respectively), and the position in theperiod-amplitude diagram both confirm that NGC 2419 is an Oosterhoff IIcluster. The average apparent magnitude of the RR Lyrae stars is <V>=20.31 +/-0.01 (sigma=0.06, 67 stars) and leads to the distance modulus (m-M)o=19.60 +/-0.05. The Color-Magnitude Diagram, reaching about 2.6 mag below the clusterturn-off, does not show clear evidence of multiple stellar populations. Clusterstars are found until r~ 10.5', and possibly as far as r~15', suggesting thatthe literature tidal radius might be underestimated. No extra-tidal structuresare clearly detected in the data. NGC 2419 has many blue stragglers and a wellpopulated horizontal branch extending from the RR Lyrae stars down to anextremely blue tail ending with the \"blue-hook\", for the first time recognizedin this cluster. The red giant branch is narrow ruling out significantmetallicity spreads. Our results seem to disfavor the interpretation of NGC2419 as either having an extragalactic origin or being the relict of a dwarfgalaxy tidally disrupted by the Milky Way.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "From photometric observations of elliptical galaxies, among which are bothradio galaxies and radio-quiet objects, an investigation was carried out of therelationship `redshift -- age of the stellar system' $(\\Delta z/\\Delta t)$. Bymeans of this relationship cosmological parameters $H(z)$ and $\\Omega_\\Lambda$are estimated. Ages of stellar systems are determined within the framework ofevolution models of synthetic spectra PEGASE and GISSEL. This approach can beconsidered as time study of objects of the early Universe independent of othercosmological models. Construction of a pooled sample is described, containing220 objects from different populations of elliptical galaxies, for which ananalysis of the upper limit of the age of formation of a stellar system wasperformed. These data were used to estimate the boundaries of determination ofthe cosmological parameters $H_0$ and $\\Lambda$--term: $H_0=72\\pm10$ and$\\Omega_\\Lambda=0.8\\pm0.1$ in the model GISSEL and $H_0=53\\pm10$, and$\\Omega_\\Lambda=0.8\\pm0.1$ in the model PEGASE.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Recent galaxy redshift surveys have brought in a large amount of accuratecosmological data out to redshift 0.3, and future surveys are expected toachieve a high degree of completeness out to a redshift exceeding 1.Consequently, a numerical programme for determining the metric of the universefrom observational data will soon become practical; and thereby realise theultimate application of Einstein's equations. Apart from detailing the cosmicgeometry, this would allow us to verify and quantify homogeneity, rather thanassuming it, as has been necessary up to now, and to do that on a metric level,and not merely at the mass distribution level. This paper is the beginning of aproject aimed at such a numerical implementation. The primary observationaldata from our past light cone consists of galaxy redshifts, apparentluminosities, angular diameters and number densities, together with sourceevolution functions, absolute luminosities, true diameters and masses ofsources. Here we start with the simplest case, that of spherical symmetry and adust equation of state, and execute an algorithm that determines the unknownmetric functions from this data. We discuss the challenges of turning thetheoretical algorithm into a workable numerical procedure, particularlyaddressing the origin and the maximum in the area distance. Our numericalmethod is tested with several artificial data sets for homogeneous andinhomogeneous models, successfully reproducing the original models. Thisdemonstrates the basic viability of such a scheme. Although current surveysdon't have sufficient completeness or accuracy, we expect this situation tochange in the near future, and in the meantime there are many refinements andgeneralisations to be added.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We study the electron spin relaxation in intrinsic and $p$-type (001) GaAsquantum wells by constructing and numerically solving the kinetic spin Blochequations. All the relevant scatterings are explicitly included, especially thespin-flip electron-heavy hole exchange scattering which leads to theBir-Aronov-Pikus spin relaxation. We show that, due to the neglection of thenonlinear terms in the electron-heavy hole exchange scattering in theFermi-golden-rule approach, the spin relaxation due to the Bir-Aronov-Pikusmechanism is greatly exaggerated at moderately high electron density and lowtemperature in the literature. We compare the spin relaxation time due to theBir-Aronov-Pikus mechanism with that due to the D'yakonov-Perel' mechanismwhich is also calculated from the kinetic spin Bloch equations with all thescatterings, especially the spin-conserving electron-electron andelectron-heavy hole scatterings, included. We find that, in intrinsic quantumwells, the effect from the Bir-Aronov-Pikus mechanism is much smaller than thatfrom the D'yakonov-Perel' mechanism at low temperature, and it is smaller by nomore than one order of magnitude at high temperature. In $p$-type quantumwells, the spin relaxation due to the Bir-Aronov-Pikus mechanism is also muchsmaller than the one due to the D'yakonov-Perel' mechanism at low temperatureand becomes comparable to each other at higher temperature when the holedensity and the width of the quantum well are large enough. We claim thatunlike in the bulk samples, the Bir-Aronov-Pikus mechanism hardly dominates thespin relaxation in two-dimensional samples.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We propose that genetic encoding of self-assembling components greatlyenhances the evolution of complex systems and provides an efficient platformfor inductive generalization, i.e. the inductive derivation of a solution to aproblem with a potentially infinite number of instances from a limited set oftest examples. We exemplify this in simulations by evolving scalable circuitryfor several problems. One of them, digital multiplication, has been intensivelystudied in recent years, where hitherto the evolutionary design of onlyspecific small multipliers was achieved. The fact that this and other problemscan be solved in full generality employing self-assembly sheds light on theevolutionary role of self-assembly in biology and is of relevance for thedesign of complex systems in nano- and bionanotechnology.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Data mining is a useful decision support technique that can be used todiscover production rules in warehouses or corporate data. Data mining researchhas made much effort to apply various mining algorithms efficiently on largedatabases. However, a serious problem in their practical application is thelong processing time of such algorithms. Nowadays, one of the key challenges isto integrate data mining methods within the framework of traditional databasesystems. Indeed, such implementations can take advantage of the efficiencyprovided by SQL engines. In this paper, we propose an integrating approach fordecision trees within a classical database system. In other words, we try todiscover knowledge from relational databases, in the form of production rules,via a procedure embedding SQL queries. The obtained decision tree is defined bysuccessive, related relational views. Each view corresponds to a givenpopulation in the underlying decision tree. We selected the classical InductionDecision Tree (ID3) algorithm to build the decision tree. To prove that ourimplementation of ID3 works properly, we successfully compared the output ofour procedure with the output of an existing and validated data miningsoftware, SIPINA. Furthermore, since our approach is tuneable, it can begeneralized to any other similar decision tree-based method.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We study the potential of the CNGS beam in constraining the parameter spaceof a model with one sterile neutrino separated from three active ones by an$\\mathcal{O}(\\eVq)$ mass-squared difference, $\\Dmq_\\Sbl$. We perform ouranalysis using the OPERA detector as a reference (our analysis can be upgradedincluding a detailed simulation of the ICARUS detector). We point out that thechannel with the largest potential to constrain the sterile neutrino parameterspace at the CNGS beam is $\\nu_\\mu \\to \\nu_\\tau$. The reason for that istwofold: first, the active-sterile mixing angle that governs this oscillationis the less constrained by present experiments; second, this is the signal forwhich both OPERA and ICARUS have been designed, and thus benefits from anextremely low background. In our analysis we also took into account $\\nu_\\mu\\to \\nu_e$ oscillations. We find that the CNGS potential to look for sterileneutrinos is limited with nominal intensity of the beam, but it issignificantly enhanced with a factor 2 to 10 increase in the neutrino flux.Data from both channels allow us, in this case, to constrain further thefour-neutrino model parameter space. Our results hold for any value of$\\Dmq_\\Sbl \\gtrsim 0.1 \\eVq$, \\textit{i.e.} when oscillations driven by thismass-squared difference are averaged. We have also checked that the bound on$\\theta_{13}$ that can be put at the CNGS is not affected by the possibleexistence of sterile neutrinos.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Pinpointing the progenitors of long duration gamma-ray bursts (LGRBs) remainsan extremely important question, although it is now clear that at least afraction of LGRBs originate in the core collapse of massive stars in type Icsupernovae, the pathways to the production of these stars, and their initialmasses, remain uncertain. Rotation is thought to be vital in the creation ofLGRBs, and it is likely that black hole creation is also necessary. We suggestthat these two constraints can be met if the GRB progenitors are very massivestars (>20 solar masses) and are formed in tight binary systems. Using simplemodels we compare the predictions of this scenario with observations and findthat the location of GRBs on their host galaxies are suggestive ofmain-sequence masses in excess of 20 solar masses, while 50% of the knowncompact binary systems may have been sufficiently close to have had thenecessary rotation rates for GRB creation. Thus, massive stars in compactbinaries are a likely channel for at least some fraction of LGRBs.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Prices of commodities or assets produce what is called time-series. Differentkinds of financial time-series have been recorded and studied for decades.Nowadays, all transactions on a financial market are recorded, leading to ahuge amount of data available, either for free in the Internet or commercially.Financial time-series analysis is of great interest to practitioners as well asto theoreticians, for making inferences and predictions. Furthermore, thestochastic uncertainties inherent in financial time-series and the theoryneeded to deal with them make the subject especially interesting not only toeconomists, but also to statisticians and physicists. While it would be aformidable task to make an exhaustive review on the topic, with this review wetry to give a flavor of some of its aspects.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Electrons in solids have been conventionally classified as either band-likeitinerant ones or atomic-like localized ones depending on their properties. Forheavy Fermion (HF) compounds, however, the f electrons show both itinerant andlocalized behaviours depending on temperature. Above the characteristictemperature T*, which is typically of the order of few K to few tens K, theirmagnetic properties are well described by the ionic f-electron models,suggesting that the f-electrons behave as 'localized' electrons. On the otherhand, well below T*, their Fermi surfaces (FS's) have been observed bymagneto-oscillatory techniques, and generally they can be explained well by the'itinerant' f-electron model. These two models assume totally different naturesof felectrons, and how they transform between localized and itinerant state asa function of temperatures has never been understood on the level of theirelectronic structures. Here we have studied the band structure of the HFantiferromagnetic superconductor UPd2Al3 well below and above T* byangle-resolved photoelectron spectroscopy (ARPES), and revealed the temperaturedependence of the electronic structure. We have found that the f-bands, whichform the FS's at low temperatures are excluded from FS's at high temperatures.The present results demonstrate how the same f-electrons show both itinerantand localized behaviours on the level of electronic structure, and provide animportant information for the unified description of the localized anditinerant nature of HF compounds.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "If the binding energy of the pulsar's surface is not so high (the case of aneutron star), both the negative and positive charges will flow out freely fromthe surface of the star. The annular free flow model for $\\gamma$-ray emissionof pulsars is suggested in this paper. It is emphasized that: (1). Two kinds ofacceleration regions (annular and core) need to be taken into account. Theannular acceleration region is defined by the magnetic field lines that crossthe null charge surface within the light cylinder. (2). If the potential dropin the annular region of a pulsar is high enough (normally the cases of youngpulsars), charges in both the annular and the core regions could be acceleratedand produce primary gamma-rays. Secondary pairs are generated in both regionsand stream outwards to power the broadband radiations. (3). The potential dropin the annular region grows more rapidly than that in the core region. Theannular acceleration process is a key point to produce wide emission beams asobserved. (4). The advantages of both the polar cap and outer gap models areretained in this model. The geometric properties of the $\\gamma$-ray emissionfrom the annular flow is analogous to that presented in a previous work by Qiaoet al., which match the observations well. (5). Since charges with differentsigns leave the pulsar through the annular and the core regions, respectively,the current closure problem can be partially solved.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The two-body interaction in dilute solutions of polymer chains in goodsolvents can be modeled by means of effective bounded potentials, the simplestof which being that of penetrable spheres (PSs). In this paper we construct twosimple analytical theories for the structural properties of PS fluids: alow-temperature (LT) approximation, that can be seen as an extension to PSs ofthe well-known solution of the Percus-Yevick (PY) equation for hard spheres,and a high-temperature (HT) approximation based on the exact asymptoticbehavior in the limit of infinite temperature. Monte Carlo simulations for awide range of temperatures and densities are performed to assess the validityof both theories. It is found that, despite their simplicity, the HT and LTapproximations exhibit a fair agreement with the simulation data within theirrespective domains of applicability, so that they complement each other. Acomparison with numerical solutions of the PY and the hypernetted-chainapproximations is also carried out, the latter showing a very good performance,except inside the core at low temperatures.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The aim of the KArlsruhe TRItium Neutrino experiment KATRIN is thedetermination of the absolute neutrino mass scale down to 0.2 eV, withessentially smaller model dependence than from cosmology and neutrinolessdouble beta decay. For this purpose, the integral electron energy spectrum ismeasured close to the endpoint of molecular tritium beta decay. The endpoint,together with the neutrino mass, should be fitted from the KATRIN data as afree parameter. The right-handed couplings change the electron energy spectrumclose to the endpoint, therefore they have some effect also to the preciseneutrino mass determination. The statistical calculations show that, using theendpoint as a free parameter, the unaccounted right-handed couplingsconstrained by many beta decay experiments can change the fitted neutrino massvalue, relative to the true neutrino mass, by not larger than about 5-10 %.Using, incorrectly, the endpoint as a fixed input parameter, the above changeof the neutrino mass can be much larger, order of 100 %, and for some cases itcan happen that for large true neutrino mass value the fitted neutrino masssquared is negative. Publications using fixed endpoint and presenting largeright-handed coupling effects to the neutrino mass determination are notrelevant for the KATRIN experiment.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The development and progress of the studies of winds and mass loss from hotstars, from about 1965 up to now, is discussed in a personal historicalperspective. The present state of knowledge about stellar winds, based onpapers presented at this workshop, is described. About ten years ago themechanisms of the winds were reasonably well understood, the mass loss rateswere known, and the predictions of stellar evolution theory with mass lossagreed with observations. However, recent studies especially those based onFUSE observations, have resulted in a significant reduction of the mass lossrates, that disagrees with predictions from radiation driven wind models. Thesituation is discussed and future studies that can clarify the situation aresuggested.  I also discuss what is known about the dissolution of star clusters indifferent environments. The dissolution time can be derived from the mass andage distributions of cluster samples. The resulting dissolution times ofclusters in the solar neighborhood (SN) and in interacting galaxies are shorterthan predicted by two-body relaxation of clusters in a tidal field. Encounterswith giant molecular clouds can explain the fate of clusters in the SN and arethe most likely cause of the short lifetime of clusters in interactinggalaxies.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Aiming at a better understand of the physical and chemical processes in thehot molecular core stage of high-mass star formation, we observed theprototypical hot core G29.96-0.02 in the 862mu band with the SubmillimeterArray (SMA) at sub-arcsecond spatial resolution. The observations resolved thehot molecular core into six submm continuum sources with the finest spatialresolution of 0.36''x0.25'' (~1800AU) achieved so far. Four of them locatedwithin 7800(AU)^2 comprise a proto-Trapezium system with estimated protostellardensities of 1.4x0^5 protostars/pc^3. The plethora of ~80 spectral lines allowsus to study the molecular outflow(s), the core kinematics, the temperaturestructure of the region as well as chemical effects. The derived hot coretemperatures are of the order 300K. We find interesting chemical spatialdifferentiations, e.g., C34S is deficient toward the hot core and is enhancedat the UCHII/hot core interface, which may be explained by temperaturesensitive desorption from grains and following gas phase chemistry. TheSiO(8-7) emission outlines likely two molecular outflows emanating from thishot core region. Emission from most other molecules peaks centrally on the hotcore and is not dominated by any individual submm peak. Potential reasons forthat are discussed. A few spectral lines that are associated with the mainsubmm continuum source, show a velocity gradient perpendicular to thelarge-scale outflow. Since this velocity structure comprises three of thecentral protostellar sources, this is not a Keplerian disk. While the data areconsistent with a gas core that may rotate and/or collapse, we cannot excludethe outflow(s) and/or nearby expanding UCHII region as possible alternativecauses of this velocity pattern.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "In a data warehousing process, the data preparation phase is crucial.Mastering this phase allows substantial gains in terms of time and performancewhen performing a multidimensional analysis or using data mining algorithms.Furthermore, a data warehouse can require external data. The web is a prevalentdata source in this context, but the data broadcasted on this medium are veryheterogeneous. We propose in this paper a UML conceptual model for a complexobject representing a superclass of any useful data source (databases, plaintexts, HTML and XML documents, images, sounds, video clips...). The translationinto a logical model is achieved with XML, which helps integrating all thesediverse, heterogeneous data into a unified format, and whose schema definitionprovides first-rate metadata in our data warehousing context. Moreover, webenefit from XML's flexibility, extensibility and from the richness of thesemi-structured data model, but we are still able to later map XML documentsinto a database if more structuring is needed.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "This paper includes a reflection on the role of networks in the study ofEnglish language acquisition, as well as a collection of practical criteria toannotate free-speech corpora from children utterances. At the theoreticallevel, the main claim of this paper is that syntactic networks should beinterpreted as the outcome of the use of the syntactic machinery. Thus, theintrinsic features of such machinery are not accessible directly from (known)network properties. Rather, what one can see are the global patterns of its useand, thus, a global view of the power and organization of the underlyinggrammar. Taking a look into more practical issues, the paper examines how tobuild a net from the projection of syntactic relations. Recall that, as opposedto adult grammars, early-child language has not a well-defined concept ofstructure. To overcome such difficulty, we develop a set of systematic criteriaassuming constituency hierarchy and a grammar based on lexico-thematicrelations. At the end, what we obtain is a well defined corpora annotation thatenables us i) to perform statistics on the size of structures and ii) to builda network from syntactic relations over which we can perform the standardmeasures of complexity. We also provide a detailed example.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The main result of this article is the fact that the currents defined byLevin give a description of the polylogarithm of an abelian scheme at thetopological level. This result was a conjecture of Levin. This provides amethod to explicit the Eisenstein classes of an abelian scheme at thetopological level. These classes are of special interest since they have amotivic origin by a theorem of Kings. In a forthcoming article, we use the mainresult of this paper to prove that the Eisenstein classes of the universalabelian scheme over an Hilbert-Blumenthal variety degenerate at the boundary ofthe Baily-Borel compactification of the base in a special value of an$L$-function associated to the underlying totally real number field. As acorollary, we get a non vanishing result for some of these Eisenstein classesin this geometric situation.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We investigate the use of optical variability to identify and study ActiveGalactic Nuclei (AGN) in the GOODS-South field. A sample of 22 mid-infraredpower law sources and 102 X-ray sources with optical counterparts in the HSTACS images were selected. Each object is classified with a variabilitysignificance value related to the standard deviation of its magnitude in fiveepochs separated by 45-day intervals. The variability significance is comparedto the optical, mid-IR, and X-ray properties of the sources. We find that 26%of all AGN candidates (either X-ray- or mid-IR-selected) are optical variables.The fraction of optical variables increases to 51% when considering sourceswith soft X-ray band ratios. For the mid-IR AGN candidates which havemultiwavelength SEDs, we find optical variability for 64% of those classifiedwith SEDs like Broad Line AGNs. While mostly unobscured AGN appear to have themost significant optical variability, some of the more obscured AGNs are alsoobserved as variables. In particular, we find two mid-IR power law-selected AGNcandidates without X-ray emission that display optical variability, confirmingtheir AGN nature.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "In this paper we consider magnetic Schr\\\"odinger operators in R^n, n \\ge 3.Under almost optimal conditions on the potentials in terms of decay andregularity we prove smoothing and Strichartz estimates, as well as a limitingabsorption principle. For large gradient perturbations the latter is not acorollary of the free case as the differentiated free resolvent does not havesmall operator norm on any weighted L^2 spaces.  We instead show that the spectral radius of such operators decreases to zero,hence their perturbation of the identity is still invertible. The key estimatesare based on an angular decomposition of the free resolvent, or rather a boundthat holds uniformly for all possible angular decompositions. The proof avoidsthe Fourier transform and instead uses H\\\"ormander's variable coefficientPlancherel theorem for oscillatory integrals.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We constrain blastwave parameters and the circumburst media of a subsample often BeppoSAX Gamma-Ray Bursts. For this sample we derive the values of theinjected electron energy distribution index, p, and the density structure indexof the circumburst medium, k, from simultaneous spectral fits to their X-ray,optical and nIR afterglow data. The spectral fits have been done in count spaceand include the effects of metallicity, and are compared with the previouslyreported optical and X-ray temporal behaviour. Using the blastwave model andsome assumptions which include on-axis viewing and standard jet structure,constant blastwave energy and no evolution of the microphysical parameters, wefind a mean value of p for the sample as a whole of 2.04 +0.02/-0.03. Astatistical analysis of the distribution demonstrates that the p values in thissample are inconsistent with a single universal value for p at the 3-sigmalevel or greater, which has significant implications for particle accelerationmodels. This approach provides us with a measured distribution of circumburstdensity structures rather than considering only the cases of k=0 (homogeneous)and k=2 (wind-like). We find five GRBs for which k can be well constrained, andin four of these cases the circumburst medium is clearly wind-like. The fifthsource has a value of 0<k<1, consistent with a homogeneous circumburst medium.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "In this work we compare and characterize the behavior of Langevin andDissipative Particle Dynamics (DPD) thermostats in a broad range ofnon-equilibrium simulations of polymeric systems. Polymer brushes in relativesliding motion, polymeric liquids in Poiseuille and Couette flows, andbrush-melt interfaces are used as model systems to analyze the efficiency andlimitations of different Langevin and DPD thermostat implementations. Widelyused coarse-grained bead-spring models under good and poor solvent conditionsare employed to assess the effects of the thermostats. We consideredequilibrium, transient, and steady state examples for testing the ability ofthe thermostats to maintain constant temperature and to reproduce theunderlying physical phenomena in non-equilibrium situations. The commonpractice of switching-off the Langevin thermostat in the flow direction is alsocritically revisited. The efficiency of different weight functions for the DPDthermostat is quantitatively analyzed as a function of the solvent quality andthe non-equilibrium situation.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We report discovery of a compact object at high Galactic latitude. The objectwas initially identified as a ROSAT All-Sky Survey Bright Source Catalog X-raysource, 1RXS J141256.0+792204, statistically likely to possess a high X-ray tooptical flux ratio. Further observations using {\\em  Swift}, Gemini-North, and the Chandra X-ray Observatory refined the sourceposition and confirmed the absence of any optical counterpart to an X-ray tooptical flux ratio of F_X/F_V > 8700 (3 sigma). Interpretation of 1RXSJ141256.0+792204 -- which we have dubbed Calvera -- as a typical X-ray-dimisolated neutron star would place it at z ~ 5.1 kpc above the Galactic disk --in the Galactic halo -- implying that it either has an extreme space velocity(v_z >~ 5100 km s-1) or has failed to cool according to theoreticalpredictions. Interpretations as a persistent anomalous X-ray pulsar, or a``compact central object'' present conflicts with these classes' typicalproperties. We conclude the properties of Calvera are most consistent withthose of a nearby (80 to 260 pc) radio pulsar, similar to the radio millisecondpulsars of 47 Tuc, with further observations required to confirm thisclassification. If it is a millisecond pulsar, it has an X-ray flux equal tothe X-ray brightest millisecond pulsar (and so is tied for highest flux); isthe closest northern hemisphere millisecond pulsar; and is potentially theclosest known millisecond pulsar in the sky, making it an interesting targetfor X-ray-study, a radio pulsar timing array, and LIGO.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "All possible transformations from the Robertson-Walker metric to thoseconformal to the Lorentz-Minkowski form are derived. It is demonstrated thatthe commonly known family of transformations and associated conformal factorsare not exhaustive and that there exists another relatively less well knownfamily of transformations with a different conformal factor in the particularcase that K = -1. Simplified conformal factors are derived for the special caseof maximally-symmetric spacetimes. The full set of all possiblecosmologically-compatible conformal forms is presented as a comprehensivetable. A product of the analysis is the determination of the set-theoreticalrelationships between the maximally symmetric spacetimes, the Robertson-Walkerspacetimes, and functionally more general spacetimes. The analysis is precededby a short historical review of the application of conformal metrics toCosmology.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present the discovery of two very-high-energy gamma-ray sources in anongoing systematic search for emission above 100 GeV from pulsar wind nebulaein survey data from the H.E.S.S. telescope array. Imaging Atmospheric CherenkovTelescopes are ideal tools for searching for extended emission from pulsar windnebulae in the very-high-energy regime. H.E.S.S., with its large field of viewof 5 degrees and high sensitivity, gives new prospects for the search for theseobjects. An ongoing systematic search for very-high-energy emission fromenergetic pulsars over the region of the Galactic plane between -60 degrees < l< 30 degrees, -2 degrees < b < 2 degrees is performed. For the resultingcandidates, the standard H.E.S.S. analysis was applied and a search formulti-wavelength counterparts was performed. We present the discovery of twonew candidate gamma-ray pulsar wind nebulae, HESS J1718-385 and HESS J1809-193.H.E.S.S. has proven to be a suitable instrument for pulsar wind nebulasearches.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "An easily implementable path solution algorithm for 2D spatial problems,based on excitable/programmable characteristics of a specific cellularnonlinear network (CNN) model is presented and numerically investigated. Thenetwork is a single layer bioinspired model which was also implemented in CMOStechnology. It exhibits excitable characteristics with regionally bistablecells. The related response realizes propagations of trigger autowaves, wherethe excitable mode can be globally preset and reset. It is shown that, obstacledistributions in 2D space can also be directly mapped onto the coupled cellarray in the network. Combining these two features, the network model can serveas the main block in a 2D path computing processor. The related algorithm andconfigurations are numerically experimented with circuit level parameters andperformance estimations are also presented. The simplicity of the model alsoallows alternative technology and device level implementation, which may becomecritical in autonomous processor design of related micro or nanoscale roboticapplications.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "This paper is the continuation of a previous one [L. {\\v{S}}amaj and B.Jancovici, 2007 {\\it J. Stat. Mech.} P02002]; for a nearly classical quantumfluid in a half-space bounded by a plain plane hard wall (no image forces), wehad generalized the Wigner-Kirkwood expansion of the equilibrium statisticalquantities in powers of Planck's constant $\\hbar$. As a model system for a moredetailed study, we consider the quantum two-dimensional one-component plasma: asystem of charged particles of one species, interacting through the logarithmicCoulomb potential in two dimensions, in a uniformly charged background ofopposite sign, such that the total charge vanishes. The corresponding classicalsystem is exactly solvable in a variety of geometries, including the presentone of a half-plane, when $\\beta e^2=2$, where $\\beta$ is the inversetemperature and $e$ is the charge of a particle: all the classical $n$-bodydensities are known. For the quantum one-component plasma, two sum rulesinvolving the truncated two-body density (and, for one of them, the densityprofile) have been derived, a long time ago, by heuristic macroscopicarguments: one sum rule is about the asymptotic form along the wall of thetruncated two-body density, the other one is about the dipole moment of thestructure factor. In the two-dimensional case at $\\beta e^2=2$, we have nowexplicit expressions up to order $\\hbar^2$ of these two quantum densities, thuswe can microscopically check the sum rules at this order. The checks arepositive, reinforcing the idea that the sum rules are correct.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present a scaling law that predicts the values of the stresses obtained innumerical simulations of saturated MRI-driven turbulence in non-stratifiedshearing boxes. It relates the turbulent stresses to the strength of thevertical magnetic field, the sound speed, the vertical size of the box, and thenumerical resolution and predicts accurately the results of 35 numericalsimulations performed for a wide variety of physical conditions. We use ourresult to show that the saturated stresses in simulations with zero netmagnetic flux depend linearly on the numerical resolution and would becomenegligible if the resolution were set equal to the natural dissipation scale inastrophysical disks. We conclude that, in order for MRI-driven turbulentangular momentum transport to be able to account for the large value of theeffective alpha viscosity inferred observationally, the disk must be threadedby a significant vertical magnetic field and the turbulent magnetic energy mustbe in near equipartition with the thermal energy. This result has importantimplications for the spectra of accretion disks and their stability.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present the latest catalog of more than 1200 spectroscopically-selectedclose binary systems observed with the Sloan Digital Sky Survey through DataRelease Five. We use the catalog to search for magnetic white dwarfs incataclysmic variable progenitor systems. Given that approximately 25% ofcataclysmic variables contain a magnetic white dwarf, and that our large sampleof close binary systems should contain many progenitors of cataclysmicvariables, it is quite surprising that we find only two potential magneticwhite dwarfs in this sample. The candidate magnetic white dwarfs, if confirmed,would possess relatively low magnetic field strengths (B_WD < 10 MG) that aresimilar to those of intermediate-Polars but are much less than the averagefield strength of the current Polar population. Additional observations ofthese systems are required to definitively cast the white dwarfs as magnetic.Even if these two systems prove to be the first evidence of detached magneticwhite dwarf + M dwarf binaries, there is still a large disparity between theproperties of the presently known cataclysmic variable population and thepresumed close binary progenitors.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "An extensive set of optical and NIR photometry and low-resolution spectra theType Ia supernova (SN Ia) 2003du was obtained using a number of facilities. Theobservations started 13 days before B-band maximum light and continued for 480days with exceptionally good time sampling. The optical photometry wascalibrated through the S-correction technique.  The UBVRIJHK light curves and the color indices of SN 2003du closely resemblethose of normal SNe Ia. SN 2003du reached a B-band maximum of 13.49 (+/-0.02)mag on JD2452766.38 (+/-0.5). We derive a B-band stretch parameter of 0.988(+/-0.003), which corresponds to dM15=1.02 (+/-0.05), indicative of a SN Ia ofstandard luminosity. The reddening in the host galaxy was estimated by threemethods, and was consistently found to be negligible. We estimate a distancemodulus of 32.79 (+/-0.15) mag to the host galaxy, UGC 9391. The peak UVOIRbolometric luminosity of 1.35(+/-0.20) 10^43 erg/s and Arnett's rule impliesthat M(Ni56)=0.68 (+/-0.14)M_sun of Ni56 was synthesized during the explosion.Modeling of the UVOIR bolometric light curve also indicates M(Ni56) in therange 0.6-0.8 M_sun. The spectral evolution of SN 2003du at both optical andNIR wavelengths also closely resembles normal SNe Ia. In particular, the Si IIratio at maximum R(Si II)=0.22 (+/-0.02) and the time evolution of theblueshift velocities of the absorption line minima are typical. The pre-maximumspectra of SN 2003du showed conspicuous high-velocity features in the Ca II H&Kdoublet and infrared triplet, and possibly in Si II 6355, lines. We compare thetime evolution of the profiles of these lines with other well-observed SNe Iaand we suggest that the peculiar pre-maximum evolution of Si II 6355 line inmany SNe Ia is due to the presence of two blended absorption components.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The extended Hubbard Hamiltonian is a widely accepted model for uncoveringthe effects of strong correlations on the phase diagram of low-dimensionalsystems, and a variety of theoretical techniques have been applied to it. Inthis paper the world-line quantum Monte Carlo method is used to study spin,charge, and bond order correlations of the one-dimensional extended Hubbardmodel in the presence of coupling to the lattice. A static alternating latticedistortion (the ionic Hubbard model) leads to enhanced charge density wavecorrelations at the expense of antiferromagnetic order. When the latticedegrees of freedom are dynamic (the Hubbard-Holstein model), we show that asimilar effect occurs even though the charge asymmetry must arisespontaneously. Although the evolution of the total energy with lattice couplingis smooth, the individual components exhibit sharp crossovers at the phaseboundaries. Finally, we observe a tendency for bond order in the region betweenthe charge and spin density wave phases.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "[Abridged] In galactic nuclei with sufficiently short relaxation times,binary supermassive black holes can evolve beyond their stalling radii viacontinued interaction with stars. We study this \"collisional\" evolutionaryregime using both fully self-consistent N-body integrations and approximateFokker-Planck models. The N-body integrations employ particle numbers up to0.26M and a direct-summation potential solver; close interactions involving thebinary are treated using a new implementation of the Mikkola-Aarseth chainregularization algorithm. Even at these large values of N, two-body scatteringoccurs at high enough rates in the simulations that they can not be simplyscaled to the large-N regime of real galaxies. The Fokker-Planck model is usedto bridge this gap; it includes, for the first time, binary-induced changes inthe stellar density and potential. The Fokker-Planck model is shown toaccurately reproduce the results of the N-body integrations, and is thenextended to the much larger N regime of real galaxies. Analytic expressions arederived that accurately reproduce the time dependence of the binary semi-majoraxis as predicted by the Fokker-Planck model. Gravitational wave coalescence isshown to occur in <10 Gyr in nuclei with velocity dispersions below about 80km/s. Formation of a core results from a competition between ejection of starsby the binary and re-supply of depleted orbits via two-body scattering. Massdeficits as large as ~4 times the binary mass are produced before coalescence.After the two black holes coalesce, a Bahcall-Wolf cusp appears around thesingle hole in one relaxation time, resulting in a nuclear density profileconsisting of a flat core with an inner, compact cluster, similar to what isobserved at the centers of low-luminosity spheroids.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present new multi-wavelength millimeter interferometric observations ofthe Herbig Ae star HD 163296 obtained with the IRAM/PBI, SMA and VLA arraysboth in continuum and in the 12CO, 13CO and C18O emission lines. Gas and dustproperties have been obtained comparing the observations with self-consistentdisk models for the dust and CO emission. The circumstellar disk is resolvedboth in the continuum and in CO. We find strong evidence that the circumstellarmaterial is in Keplerian rotation around a central star of 2.6 Msun. The diskinclination with respect to the line of sight is 46+-4 deg with a positionangle of 128+-4 deg. The slope of the dust opacity measured between 0.87 and 7mm (beta=1) confirms the presence of mm/cm-size grains in the disk midplane.The dust continuum emission is asymmetric and confined inside a radius of 200AU while the CO emission extends up to 540 AU. The comparison between dust andCO temperature indicates that CO is present only in the disk interior. Finally,we obtain an increasing depletion of CO isotopomers from 12CO to 13CO and C18O.We argue that these results support the idea that the disk of HD 163296 isstrongly evolved. In particular, we suggest that there is a strong depletion ofdust relative to gas outside 200 AU; this may be due to the inward migration oflarge bodies that form in the outer disk or to clearing of a large gap in thedust distribution by a low mass companion.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We model energy dependencies of the quasi periodic oscillations (QPO) in themodel of disc epicyclic motions, with X-ray modulation caused by varyingrelativistic effects. The model was proposed to explain the high frequency QPOobserved in X-ray binaries. We consider two specific scenarios for the geometryof accretion flow and spectral formation. Firstly, a standard cold accretiondisc with an active X-ray emitting corona is assumed to oscillate. Secondly,only a hot X-ray emitting accretion flow oscillates, while the cold disc isabsent at the QPO radius. We find that the QPO spectra are generally similar tothe spectrum of radiation emitted at the QPO radius, and they are broadened bythe relativistic effects. In particular, the QPO spectrum contains the disccomponent in the oscillating disc with a corona scenario. We also review theavailable data on energy dependencies of high frequency QPO, and we point outthat they appear to lack the disc component in their energy spectra. This wouldsuggest the hot flow geometry in the spectral states when high frequency QPOare observed.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "A study of the $p d \\to p d \\eta$ reaction in the energy range where therecent data from Uppsala are available, is done in the two-step model of $\\eta$production including the final state interaction. The $\\eta -d$ final stateinteraction is incorporated through the solution of the Lippmann Schwingerequation using an elastic scattering matrix element, $T_{\\eta d \\to \\eta d}$,which is required to be half off-shell. It is written in a factorized form,with an off-shell form factor multiplying an on-shell part given by aneffective range expansion up to the fourth power in momentum. The parameters ofthis expansion have been taken from an existing recent relativistic Faddeevequation solution for the $\\eta NN$ system corresponding to different $\\eta-N$scattering amplitudes. Calculations have also been done using few bodyequations within a finite rank approximation (FRA) to generate $T_{\\eta d \\to\\eta d}$. The $p-d$ final state interaction is included in the spirit of theWatson-Migdal prescription by multiplying the matrix element by the inverse ofthe Jost function. The $\\eta-d$ interaction is found to be dominant in theregion of small invariant $\\eta -d$ mass, $M_{\\eta d}$. The $p-d$ interactionenhances the cross section in the whole region of $M_{\\eta d}$, but is largerfor large $M_{\\eta d}$. We find nearly isotropic angular distributions of theproton and the deuteron in the final state. All the above observations are inagreement with data. The production mechanism for the entire range of theexisting data on the $p d \\to p d \\eta$ reaction seems to be dominated by thetwo-step model of $\\eta$ production.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We consider a class of real random polynomials, indexed by an integer d, oflarge degree n and focus on the number of real roots of such randompolynomials. The probability that such polynomials have no real root in theinterval [0,1] decays as a power law n^{-\\theta(d)} where \\theta(d)>0 is theexponent associated to the decay of the persistence probability for thediffusion equation with random initial conditions in space dimension d. For neven, the probability that such polynomials have no root on the full real axisdecays as n^{-2(\\theta(d) + \\theta(2))}. For d=1, this connection allows for aphysical realization of real random polynomials. We further show that theprobability that such polynomials have exactly k real roots in [0,1] has anunusual scaling form given by n^{-\\tilde \\phi(k/\\log n)} where \\tilde \\phi(x)is a universal large deviation function.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The luminosity and the spectral distribution of the afterglow of GRB 031203have been presented within our theoretical framework, which envisages the GRBstructure as composed by a proper-GRB, emitted at the transparency of anelectron-positron plasma with suitable baryon loading, and an afterglowcomprising the \"prompt emission\" as due to external shocks. In addition to theGRB emission, there appears to be a prolonged soft X-Ray emission lasting for10^6-10^7 seconds followed by an exponential decay. This additional source hasbeen called by us URCA-3. It is urgent to establish if this component isrelated to the GRB or to the Supernova (SN). In this second case, there are twopossibilities: either the interaction of the SN ejecta with the interstellarmedium or, possibly, the cooling of a young neutron star formed in the SN2003lw process. The analogies and the differences between this triptych GRB031203 / SN 2003lw / URCA-3 and the corresponding ones GRB 980425 / SN 1998bw /URCA-1 and GRB 030329 / SN 2003dh / URCA-2, as well as GRB 060218 / SN 2006ajare discussed.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "In scintillator detectors, the forward displacement of the neutron in thereaction $\\bar\\nu_e+p\\to e^++n$ provides neutrino directional information asdemonstrated by the CHOOZ reactor experiment with 2,500 events. The neardetector of the forthcoming Double Chooz experiment will collect$1.6\\times10^5$ events per year, enough to determine the average neutrinodirection with a $1 \\sigma$ half-cone aperture of $2.3^\\circ$ in one year. Itis more difficult to separate the two Chooz reactors that are viewed at aseparation angle $\\phi=30^\\circ$. If their strengths are known andapproximately equal, the azimuthal location of each reactor is obtained with$\\pm6^\\circ$ ($1 \\sigma$) and the probability of confusing them with a singlesource is less than 11%. Five year's data reduce this ``confusion probability''to less than 0.3%, i.e., a $3 \\sigma$ separation is possible. All of thesenumbers improve rapidly with increasing angular separation of the sources. Fora setup with $\\phi=90^\\circ$ and one year's data, the azimuthal $1 \\sigma$uncertainty for each source decreases to $\\pm3.2^\\circ$. Of course, for DoubleChooz the two reactor locations are known, allowing one instead to measuretheir individual one-year integrated power output to $\\pm11%$ ($1 \\sigma$), andtheir five-year integrated output to $\\pm4.8%$ ($1 \\sigma$).", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We address the inverse problem of cosmic large-scale structure reconstructionfrom a Bayesian perspective. For a linear data model, a number of known andnovel reconstruction schemes, which differ in terms of the underlying signalprior, data likelihood, and numerical inverse extra-regularization schemes arederived and classified. The Bayesian methodology presented in this paper triesto unify and extend the following methods: Wiener-filtering, Tikhonovregularization, Ridge regression, Maximum Entropy, and inverse regularizationtechniques. The inverse techniques considered here are the asymptoticregularization, the Jacobi, Steepest Descent, Newton-Raphson,Landweber-Fridman, and both linear and non-linear Krylov methods based onFletcher-Reeves, Polak-Ribiere, and Hestenes-Stiefel Conjugate Gradients. Thestructures of the up-to-date highest-performing algorithms are presented, basedon an operator scheme, which permits one to exploit the power of fast Fouriertransforms. Using such an implementation of the generalized Wiener-filter inthe novel ARGO-software package, the different numerical schemes arebenchmarked with 1-, 2-, and 3-dimensional problems including structured whiteand Poissonian noise, data windowing and blurring effects. A novel numericalKrylov scheme is shown to be superior in terms of performance and fidelity.These fast inverse methods ultimately will enable the application of samplingtechniques to explore complex joint posterior distributions. We outline how thespace of the dark-matter density field, the peculiar velocity field, and thepower spectrum can jointly be investigated by a Gibbs-sampling process. Such amethod can be applied for the redshift distortions correction of the observedgalaxies and for time-reversal reconstructions of the initial density field.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Inelastic and elastic neutron scattering is used to study spin correlationsin the quasi-one dimensional quantum antiferromagnet IPA-CuCl3 in strongapplied magnetic fields. A condensation of magnons and commensurate transverselong-range ordering is observe at a critical filed $H_c=9.5$ T. The fielddependencies of the energies and polarizations of all magnon branches areinvestigated both below and above the transition point. Their dispersion ismeasured across the entire 1D Brillouin zone in magnetic fields up to 14 T. Thecritical wave vector of magnon spectrum truncation [Masuda et al., Phys. Rev.Lett. 96, 047210 (2006)] is found to shift from h_c 0.35 at H>H_c. A drasticreduction of magnon bandwidths in the ordered phase [Garlea et al., Phys. Rev.Lett. 98, 167202 (2007)] is observed and studied in detail. New features of thespectrum, presumably related to this bandwidth collapse, are observed justabove the transition field.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "A solution is given to the following problem: how to compute themultiplicity, or more generally the Hilbert function, at a point on a Schubertvariety in an orthogonal Grassmannian. Standard monomial theory is applied totranslate the problem from geometry to combinatorics. The solution of theresulting combinatorial problem forms the bulk of the paper. This approach hasbeen followed earlier to solve the same problem for the Grassmannian and thesymplectic Grassmannian.  As an application, we present an interpretation of the multiplicity as thenumber of non-intersecting lattice paths of a certain kind.  Taking the Schubert variety to be of a special kind and the point to be the\"identity coset,\" our problem specializes to a problem about Pfaffian idealstreatments of which by different methods exist in the literature. Alsoavailable in the literature is a geometric solution when the point is a\"generic singularity.\"", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "In this paper we suggest a theoretical method based on the statisticalmechanics for treating the alpha-helix-random coil transition in alaninepolypeptides. We consider this process as a first-order phase transition anddevelop a theory which is free of model parameters and is based solely onfundamental physical principles. It describes essential thermodynamicalproperties of the system such as heat capacity, the phase transitiontemperature and others from the analysis of the polypeptide potential energysurface calculated as a function of two dihedral angles, responsible for thepolypeptide twisting. The suggested theory is general and with somemodification can be applied for the description of phase transitions in othercomplex molecular systems (e.g. proteins, DNA, nanotubes, atomic clusters,fullerenes).", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Let M be a symplectic-toric manifold of dimension at least four. This paperinvestigates the so called symplectic ball packing problem in the toralequivariant setting. We show that the set of toric symplectic ball packings ofM admits the structure of a convex polytope. Previous work of the first authorshows that up to equivalence, only CP^1 x CP^1 and CP^2 admit density onepackings when n=2 and only CP^n admits density one packings when n>2. Incontrast, we show that for a fixed n>=2 and each r in (0, 1), there areuncountably many inequivalent 2n-dimensional symplectic-toric manifolds with amaximal toric packing of density r. This result follows from a general analysisof how the densities of maximal packings change while varying a givensymplectic-toric manifold through a family of symplectic-toric manifolds thatare equivariantly diffeomorphic but not equivariantly symplectomorphic.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Astronomy can never be a hard core physics discipline, because the Universeoffers no control experiment, i.e. with no independent checks it is bound to behighly ambiguous and degenerate. Thus e.g. while superluminal motion can beexplained by Special Relativity. data on the former can never on their own beused to establish the latter. This is why traditionally astrophysicists havebeen content with (and proud of) their ability to use known physical laws andprocesses established in the laboratory to explain celestial phenomena.Cosmology is not even astrophysics: all the principal assumptions in this fieldare unverified (or unverifiable) in the laboratory, and researchers are quitecomfortable with inventing unknowns to explain the unknown. How then could,after fifty years of failed attempt in finding dark matter, the fields of darkmatter {\\it and now} dark energy have become such lofty priorities in astronomyfunding, to the detriment of all other branches of astronomy? I demonstrate inthis article that while some of is based upon truth, at least just as much of$\\Lambda$CDM cosmology has been propped by a paralyzing amount of propagandawhich suppress counter evidence and subdue competing models. The recent WMAP3paper of Spergel et al (2007) will be used as case in point on selectivecitation. I also show that when all evidence are taken into account, two of thecompeting models that abolish dark energy and/or dark matter do not trailbehind $\\Lambda$CDM by much. Given all of the above, I believe astronomy is nolonger heading towards a healthy future, unless funding agencies re-think theirmaster plans by backing away from such high a emphasis on groping in the dark.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "In recent years, the availability of highly pure stable isotopes has madepossible the investigation of the dependence of the physical properties ofcrystals, in particular semiconductors, on their isotopic composition.Following the investigation of the specific heat ($C_p$, $C_v$) of monatomiccrystals such as diamond, silicon, and germanium, similar investigations havebeen undertaken for the tetrahedral diatomic systems ZnO and GaN (wurtzitestructure), for which the effect of the mass of the cation differs from that ofthe anion. In this article we present measurements for a semiconductor withrock salt structure, namely lead sulfide. Because of the large difference inthe atomic mass of both constituents ($M_{\\rm Pb}$= 207.21 and ($M_{\\rmS}$=32.06 a.m.u., for the natural isotopic abundance) the effects of varyingthe cation and that of the anion mass are very different for this canonicalsemiconductor. We compare the measured temperature dependence of $C_p \\approxC_v$, and the corresponding derivatives with respect to ($M_{\\rm Pb}$ and$M_{\\rm S}$), with \\textit{\\textit{ab initio}} calculations based on thelattice dynamics obtained from the local density approximation (LDA) electronicband structure. Quantitative deviations between theory and experiment areattributed to the absence of spin-orbit interaction in the ABINIT program usedfor the electronic band structure calculations.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The favoured progenitors of long-duration gamma-ray bursts (GRBs) are rapidlyrotating Wolf-Rayet (WR) stars. However, most Galactic WR stars are slowrotators, as stellar winds are thought to remove angular momentum. This poses achallenge to the collapsar model. Recent observations indicate that GRBs occurpredominately in low metallicity (Z) environments, which may resolve theproblem: lower Z leads to less mass loss, which may inhibit angular momentumremoval, allowing WR stars to remain rotating rapidly until collapse. We wishto determine whether low Z WR stars rotate on average more rapidly thanGalactic WR stars, and perform a Very Large Telescope (VLT) linearspectropolarimetry survey of WR stars in the low Z environment of the LargeMagellanic Cloud (LMC) and compare our results with the Galactic sample. Wefind that only 2 out of 13 (i.e. 15%) of LMC WR stars show line polarizationeffects, compared to a similarly low fraction of ~15-20% for Galactic WR stars.The low incidence of line polarization effects in LMC WR stars suggests thatthe threshold metallicity where significant differences in WR rotationalproperties occur is below that of the LMC (Z ~ 0.5 Zsun), possibly constrainingGRB progenitor channels to this upper metallicity.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Given an object over the algebraic closure Qbar of Q, there is often noreason for invariants of the corresponding holomorphic object to be preservedby the absolute Galois group Gal(Qbar/Q), and in general this is not true,although it is sometimes surprising to observe in practice. The case of coversof the projective line branched only over the points 0, 1, and infinity,through Belyi's theorem, leads to Grothendieck's dessins d'enfants program forunderstanding the absolute Galois group through its faithful action on suchcovers. This note is motivated by Catanese's question about ahigher-dimensional analogue: does the absolute Galois group act faithfully onthe deformation equivalence classes of smooth surfaces? (These equivalenceclasses are of course by definition the strongest deformation invariants.) Wegive a short proof of a weaker result: the absolute Galois group actsfaithfully on the irreducible components of the moduli space of smooth surfaces(of general type, canonically polarized). Bauer, Catanese, and Grunewald haverecently answered Catanese's original question using a different construction.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Context: L'-band (3.8 micron) images of the Galactic Center show a largenumber of thin filaments in the mini-spiral, located west of the mini-cavityand along the inner edge of the Northern Arm. One possible mechanism that couldproduce such structures is the interaction of a central wind with themini-spiral. Additionally, we identify similar features that appear to beassociated with stars. Aims: We present the first proper motion measurements ofthe thin dust filaments observed in the central parsec around SgrA* andinvestigate possible mechanisms that could be responsible for the observedmotions. Methods: The observations have been carried out using the NACOadaptive optics system at the ESO VLT. The images have been transformed to acommon coordinate system and features of interest were extracted. Then across-correlation technique could be performed in order to determine theoffsets between the features with respect to their position in the referenceepoch. Results: We derive the proper motions of a number of filaments and 2cometary shaped dusty sources close (in projection) to SgrA*. We show that theshape and the motion of the filaments does not agree with a purely Keplerianmotion of the gas in the potential of the supermassive black hole at theposition of SgrA*. Therefore, additional mechanisms must be responsible fortheir formation and motion. We argue that the properties of the filaments areprobably related to an outflow from the disk of young mass-losing stars aroundSgrA*. In part, the outflow may originate from the black hole itself. We alsopresent some evidence and theoretical considerations that the outflow may becollimated.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "This is an overview of recent progress in constructing and studyingsuperextensions of the Landau problem of a quantum particle on a plane in theuniform magnetic field, as well as of its Haldane's $S^2$ generalization ({\\tthep-th/0311159, hep-th/0404108, hep-th/0510019, hep-th/0612300}). The mainattention is paid to the planar super Landau models which are invariant underthe inhomogeneous supergroup ISU(1|1), a contraction of the supergroup SU(2|1),and provide minimal superextensions of the original Landau model. Their commonnotable feature is the presence of a hidden dynamical worldline N=2supersymmetry. It exists at the classical and quantum levels and is revealedmost naturally while passing to the new invariant inner products in the spaceof quantum states in order to make the norms of all states positive. For one ofthe planar models, the superplane Landau model, we present an off-shellworldline superfield formulation in which the N=2 supersymmetry gets manifest.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The first-order eikonal approximation is frequently adopted in interpretingthe results of $A(e,e'p)$ measurements. Glauber calculations, for example,typically adopt the first-order eikonal approximation. We present an extensionof the relativistic eikonal approach to $A(e,e'p)$ which accounts forsecond-order eikonal corrections. The numerical calculations are performedwithin the relativistic optical model eikonal approximation. The nucleartransparency results indicate that the effect of the second-order eikonalcorrections is rather modest, even at $Q^{2} \\approx 0.2$ (GeV/c)$^2$. The sameapplies to polarization observables, left-right asymmetries, and differentialcross sections at low missing momenta. At high missing momenta, however, thesecond-order eikonal corrections are significant and bring the calculations incloser agreement with the data and/or the exact results from models adoptingpartial-wave expansions.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We investigate the behavior of the Gibbs-Shannon entropy of the stationarynonequilibrium measure describing a one-dimensional lattice gas, of L sites,with symmetric exclusion dynamics and in contact with particle reservoirs atdifferent densities. In the hydrodynamic scaling limit, L to infinity, theleading order (O(L)) behavior of this entropy has been shown by Bahadoran to bethat of a product measure corresponding to strict local equilibrium; we computethe first correction, which is O(1). The computation uses a formal expansion ofthe entropy in terms of truncated correlation functions; for this system thek-th such correlation is shown to be O(L^{-k+1}). This entropy correctiondepends only on the scaled truncated pair correlation, which describes thecovariance of the density field. It coincides, in the large L limit, with thecorresponding correction obtained from a Gaussian measure with the samecovariance.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The theory of the dislocation motion in the periodic potential relief of thecrystal lattice (the Peierls-Nabarro barriers) is reviewed. On the basis of thekink mechanism the temperature dependence of the flow stress is described for awide class of materials. The theory of quantum mechanical dislocationtunnelling through the Peierls-Nabarro barriers is extended and compared withexperimental data on the plasticity of alkali halides, BCC and HCP metals atlow temperatures. The behavior of the flow stress at the range of athermicanomalies is modeled by changing the mechanism of the dislocation motion fromthe thermally activated hopping over the barriers to the quantum tunnellingthrough them. Some results of previous calculations are represented in a moreexplicit convenient for applications form. The pronounced effect of theswitching between the normal and the superconducting states on the flow stressof metals is explained on the basis of the change in the dissipative propertiesof the electron subsystem affecting the dislocation motion.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We search for stellar and substellar companions of young nearby stars toinvestigate stellar multiplicity and formation of stellar and substellarcompanions. We detect common proper-motion companions of stars via multi-epochimaging. Their companionship is finally confirmed with photometry andspectroscopy. Here we report the discovery of a new co-moving (13 sigma)stellar companion ~17.8 arcsec (350 AU in projected separation) north of thenearby star HD141272 (21 pc). With EMMI/NTT optical spectroscopy we determinedthe spectral type of the companion to be M3+-0.5V. The derived spectral type aswell as the near infrared photometry of the companion are both fully consistentwith a 0.26+-0.07 Msol dwarf located at the distance of HD141272 (21 pc).Furthermore the photometry data rules out the pre-main sequence status, sincethe system is consistent with the ZAMS of the Pleiades.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "A system of one-dimensional Brownian motions (BMs) conditioned never tocollide with each other is realized as (i) Dyson's BM model, which is a processof eigenvalues of hermitian matrix-valued diffusion process in the Gaussianunitary ensemble (GUE), and as (ii) the $h$-transform of absorbing BM in a Weylchamber, where the harmonic function $h$ is the product of differences ofvariables (the Vandermonde determinant). The Karlin-McGregor formula givesdeterminantal expression to the transition probability density of absorbing BM.We show from the Karlin-McGregor formula, if the initial state is in theeigenvalue distribution of GUE, the noncolliding BM is a determinantal process,in the sense that any multitime correlation function is given by a determinantspecified by a matrix-kernel. By taking appropriate scaling limits, spatiallyhomogeneous and inhomogeneous infinite determinantal processes are derived. Wenote that the determinantal processes related with noncolliding particlesystems have a feature in common such that the matrix-kernels are expressedusing spectral projections of appropriate effective Hamiltonians. On the commonstructure of matrix-kernels, continuity of processes in time is proved andgeneral property of the determinantal processes is discussed.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Transport properties of ultrasmall quantum dots with a single unpairedelectron are commonly modeled by the nonequilibrium Kondo model, describing theexchange interaction of a spin-1/2 local moment with two leads ofnoninteracting electrons. Remarkably, the model possesses an exact solutionwhen tuned to a special manifold in its parameter space known as the Toulouselimit. We use the Toulouse limit to exactly calculate the adiabatically pumpedspin current in the Kondo regime. In the absence of both potential scatteringand a voltage bias, the instantaneous charge current is strictly zero for ageneric Kondo model. However, a nonzero spin current can be pumped through thesystem in the presence of a finite magnetic field, provided the spin couplesasymmetrically to the two leads. Tunneling through a Kondo impurity thus offersa natural mechanism for generating a pure spin current. We show, in particular,that one can devise pumping cycles along which the average spin pumped percycle is closely equal to $\\hbar$. By analogy with Brouwer's formula fornoninteracting systems with two driven parameters, the pumped spin current isexpressed as a geometrical property of a scattering matrix. However, therelevant %Alex: I replaced topological with geometrical in the sentence abovescattering matrix that enters the formulation pertains to the Majorana fermionsthat appear at the Toulouse limit rather than the physical electrons that carrythe current. These results are obtained by combining the nonequilibrium KeldyshGreen function technique with a systematic gradient expansion, explicitlyexposing the small parameter controlling the adiabatic limit.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We consider a simple Newtonian model of a steady accretion disk around ablack hole. The model is based on height-integrated hydrodynamic equations,alpha-viscosity, and a pseudo-Newtonian potential that results in an innermoststable circular orbit (ISCO) that closely approximates the one predicted by GR.We find that the hydrodynamic models exhibit increasing deviations from thestandard disk model of Shakura & Sunyaev as disk thickness H/R or the value ofalpha increases. The latter is an analytical model in which the viscous torqueis assumed to vanish at the ISCO. We consider the implications of the resultsfor attempts to estimate black hole spin by using the standard disk model tofit continuum spectra of black hole accretion disks. We find that the error inthe spin estimate is quite modest so long as H/R < 0.1 and alpha < 0.2. Atworst the error in the estimated value of the spin parameter is 0.1 for anon-spinning black hole; the error is much less for a rapidly spinning hole. Wealso consider the density and disk thickness contrast between the gas in thedisk and that inside the ISCO. The contrast needs to be large if black holespin is to be successfully estimated by fitting the relativistically-broadenedX-ray line profile of fluorescent iron emission from reflection off anaccretion disk. In our hydrodynamic models, the contrast in density andthickness is low when H/R>0.1, sugesting that the iron line technique may bemost reliable in extemely thin disks. We caution that these results have beenobtained with a viscous hydrodynamic model and need to be confirmed with MHDsimulations of radiatively cooled thin disks.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present experimental measurements of photodesorption from ices ofastrophysical relevance. Layers of benzene and water ice were irradiated with alaser tuned to an electronic transition in the benzene molecule. Thetranslational energy of desorbed molecules was measured by time-of-flight (ToF)mass spectrometry. Three distinct photodesorption processes were identified - adirect adsorbate-mediated desorption producing benzene molecules with atranslational temperature of around 1200 K, an indirect adsorbate-mediateddesorption resulting in water molecules with a translational temperature ofaround 450 K, and a substrate-mediated desorption of both benzene and waterproducing molecules with translational temperatures of around 530 K and 450 Krespectively. The translational temperature of each population of desorbedmolecules is well above the temperature of the ice matrix. The implications forgas-phase chemistry in the interstellar medium are discussed.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present the results of a visible spectroscopic and photometric survey ofJupiter Trojans belonging to different dynamical families carried out at theESO-NTT telescope. We obtained data on 47 objects, 23 belonging to the L5 swarmand 24 to the L4 one. These data together with those already published byFornasier et al. (2004a) and Dotto et al. (2006), constitute a total sample ofvisible spectra for 80 objects. The survey allows us to investigate sixfamilies (Aneas, Anchises, Misenus, Phereclos, Sarpedon, Panthoos) in the L5cloud and four L4 families (Eurybates, Menelaus, 1986 WD and 1986 TS6). Thesample that we measured is dominated by D--type asteroids, with the exceptionof the Eurybates family in the L4 swarm, where there is a dominance of C- andP-type asteroids. All the spectra that we obtained are featureless with theexception of some Eurybates members, where a drop--off of the reflectance isdetected shortward of 5200 A. Similar features are seen in main belt C-typeasteroids and commonly attributed to the intervalence charge transfertransition in oxidized iron. Our sample comprises fainter and smaller Trojansas compared to the literature's data and allows us to investigate theproperties of objects with estimated diameter smaller than 40--50 km. Theanalysis of the spectral slopes and colors versus the estimated diameters showsthat the blue and red objects have indistinguishable size distribution. Weperform a statistical investigation of the Trojans's spectra propertydistributions as a function of their orbital and physical parameters, and incomparison with other classes of minor bodies in the outer Solar System.Trojans at lower inclination appear significantly bluer than those at higherinclination, but this effect is strongly driven by the Eurybates family.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We report the discovery of 14 quasars in the vicinity of HE2347-4342, one ofthe two quasars whose intergalactic HeII forest has been resolved with FUSE. Byanalysing the HI and the HeII opacity variations separately, no transverseproximity effect is detected near three foreground quasars of HE2347-4342:QSOJ23503-4328 (z=2.282, $\\vartheta=3.59$ arcmin), QSOJ23500-4319 (z=2.302,$\\vartheta=8.77$ arcmin) and QSOJ23495-4338 (z=2.690, $\\vartheta=16.28$arcmin). This is primarily due to line contamination and overdensities probablycreated by large-scale structure. By comparing the HI absorption and thecorresponding HeII absorption, we estimated the fluctuating spectral shape ofthe extragalactic UV radiation field along this line of sight. We find that theUV spectral shape near HE2347-4342 and in the projected vicinity of the threeforeground quasars is statistically harder than expected from UV backgroundmodels dominated by quasars. In addition, we find three highly ionised metalline systems near the quasars. However, they do not yield further constraintson the shape of the ionising field. We conclude that the foreground quasarsshow a transverse proximity effect that is detectable as a local hardening ofthe UV radiation field, although the evidence is strongest for QSOJ23495-4338.Thus, the relative spectral hardness traces the proximity effect also inoverdense regions prohibiting the traditional detection in the HI forest.Furthermore, we emphasise that softening of quasar radiation by radiativetransfer in the intergalactic medium is important to understand the observedspectral shape variations. From the transverse proximity effect ofQSOJ23495-4338 we obtain a lower limit on the quasar lifetime of ~25 Myr.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "In almost all structure formation models, primordial perturbations arecreated within a homogeneous and isotropic universe, like the one we observe.Because their ensemble averages inherit the symmetries of the spacetime inwhich they are seeded, cosmological perturbations then happen to bestatistically isotropic and homogeneous. Certain anomalies in the cosmicmicrowave background on the other hand suggest that perturbations do notsatisfy these statistical properties, thereby challenging perhaps ourunderstanding of structure formation. In this article we relax this tension. Weshow that if the universe contains an appropriate triad of scalar fields withspatially constant but non-zero gradients, it is possible to generatestatistically anisotropic and inhomogeneous primordial perturbations, eventhough the energy momentum tensor of the triad itself is invariant undertranslations and rotations.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We study how to incorporate CP violation in the Froggatt--Nielsen (FN)mechanism. To this end, we introduce non-renormalizable interactions with aflavor democratic structure to the fermion mass generation sector. It is foundthat at least two iso-singlet scalar fields with imposed a discrete symmetryare necessary to generate CP violation due to the appearance of the relativephase between their vacuum expectation values.  In the simplest model, ratios of quark masses and theCabibbo-Kobayashi-Maskawa (CKM) matrix including the CP violating phase aredetermined by the CKM element |V_{us}| and the ratio of two vacuum expectationvalues R=|R|e^{i*alpha} (a magnitude and a phase). It is demonstrated how theangles phi_i (i=1--3) of the unitarity triangle and the CKM off-diagonalelements |V_{ub}| and |V_{cb}| are predicted as a function of |V_{us}|, |R| and\\alpha. Although the predicted value of the CP violating phase does not agreewith the experimental data within the simplest model, the basic idea of ourscenario would be promising to construct a more realistic model of flavor andCP violation.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Let $f\\in L_{2\\pi}$ be a real-valued even function with its Fourier series $\\frac{a_{0}}{2}+\\sum_{n=1}^{\\infty}a_{n}\\cos nx,$ and let $S_{n}(f,x), n\\geq1,$ be the $n$-th partial sum of the Fourier series. It is well-known that ifthe nonnegative sequence $\\{a_{n}\\}$ is decreasing and $\\lim\\limits_{n\\to\\infty}a_{n}=0$, then $$ \\lim\\limits_{n\\to \\infty}\\Vert f-S_{n}(f)\\Vert_{L}=0{if and only if} \\lim\\limits_{n\\to \\infty}a_{n}\\log n=0. $$ We weaken themonotone condition in this classical result to the so-called mean value boundedvariation ($MVBV$) condition. The generalization of the above classical resultin real-valued function space is presented as a special case of the main resultin this paper which gives the $L^{1}$% -convergence of a function $f\\inL_{2\\pi}$ in complex space. We also give results on $L^{1}$-approximation of afunction $f\\in L_{2\\pi}$ under the $% MVBV$ condition.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Rapidly oscillating potentials with a vanishing time average have been usedfor a long time to trap charged particles in source-free regions. It has beenargued that the motion of a particle in such a potential can be approximatelydescribed by a time independent effective potential, which does not depend uponthe initial phase of the oscillating potential. However, here we show that themotion of a particle and its trapping condition significantly depend upon thisinitial phase for arbitrarily high frequencies of the potential's oscillation.We explain this novel phenomenon by showing that the motion of a particle isdetermined by the effective potential stated in the literature only if itsinitial conditions are transformed according to a transformation which we showto significantly depend on the potential's initial phase for arbitrarily highfrequencies. We confirm our theoretical findings by numerical simulations.Further, we demonstrate that the found phenomenon offers new ways to manipulatethe dynamics of particles which are trapped by rapidly oscillating potentials.Finally, we propose a simple experiment to verify the theoretical findings ofthis work.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The HARPS high-resolution high-accuracy spectrograph is offered to theastronomical community since the second half of 2003. Since then, we have beenusing this instrument for monitoring radial velocities of a large sample ofSolar-type stars (~1400 stars) in order to search for their possible low-masscompanions. Amongst the goals of our survey, one is to significantly increasethe number of detected extra-solar planets in a volume-limited sample toimprove our knowledge of their orbital elements distributions and thus obtainbetter constraints for planet-formation models.  In this paper, we present the HARPS radial-velocity data and orbitalsolutions for 3 Solar-type stars: HD 100777, HD 190647, and HD 221287. Theradial-velocity data of HD 100777 is best explained by the presence of a 1.1M_Jup planetary companion on a 384--day eccentric orbit (e=0.36). The orbitalfit obtained for the slightly evolved star HD 190647 reveals the presence of along-period (P=1038 d) 1.9 M_Jup planetary companion on a moderately eccentricorbit (e=0.18). HD 221287 is hosting a 3.1 M_Jup planet on a 456--day orbit.The shape of this orbit is not very well constrained because of our non-optimaltemporal coverage and because of the presence of abnormally large residuals. Wefind clues for these large residuals to result from spectral line profilevariations probably induced by stellar activity related processes.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "It is known that within the interacting electron model Hamiltonian for theone-dimensional 1/4-filled band, the singlet ground state is a Wigner crystalonly if the nearest neighbor electron-electron repulsion is larger than acritical value. We show that this critical nearest neighbor Coulomb interactionis different for each spin subspace, with the critical value decreasing withincreasing spin. As a consequence, with the lowering of temperature, there canoccur a transition from a Wigner crystal charge-ordered state to a spin-Peierlsstate that is a Bond-Charge-Density Wave with charge occupancies different fromthe Wigner crystal. This transition is possible because spin excitations fromthe spin-Peierls state in the 1/4-filled band are necessarily accompanied bychanges in site charge densities. We apply our theory to the 1/4-filled bandquasi-one-dimensional organic charge-transfer solids in general and to 2:1tetramethyltetrathiafulvalene (TMTTF) and tetramethyltetraselenafulvalene(TMTSF) cationic salts in particular. We believe that many recent experimentsstrongly indicate the Wigner crystal to Bond-Charge-Density Wave transition inseveral members of the TMTTF family. We explain the occurrence of two differentantiferromagnetic phases but a single spin-Peierls state in the generic phasediagram for the 2:1 cationic solids. The antiferromagnetic phases can haveeither the Wigner crystal or the Bond-Charge-Spin-Density Wave chargeoccupancies. The spin-Peierls state is always a Bond-Charge-Density Wave.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Numerical simulations of Milky-Way size Cold Dark Matter (CDM) halos predicta steeply rising mass function of small dark matter subhalos and a substructurecount that greatly outnumbers the observed satellites of the Milky Way. Severalproposed explanations exist, but detailed comparison between theory andobservation in terms of the maximum circular velocity (Vmax) of the subhalos ishampered by the fact that Vmax for satellite halos is poorly constrained. Wepresent comprehensive mass models for the well-known Milky Way dwarfsatellites, and derive likelihood functions to show that their masses within0.6 kpc (M_0.6) are strongly constrained by the present data. We show that theM_0.6 mass function of luminous satellite halos is flat between ~ 10^7 and 10^8M_\\odot. We use the ``Via Lactea'' N-body simulation to show that the M_0.6mass function of CDM subhalos is steeply rising over this range. We rule outthe hypothesis that the 11 well-known satellites of the Milky Way are hosted bythe 11 most massive subhalos. We show that models where the brightestsatellites correspond to the earliest forming subhalos or the most massiveaccreted objects both reproduce the observed mass function. A similar analysiswith the newly-discovered dwarf satellites will further test these scenariosand provide powerful constraints on the CDM small-scale power spectrum and warmdark matter models.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We study the intersection points of a fixed planar curve $\\Gamma$ with thenodal set of a translationally invariant and isotropic Gaussian random field$\\Psi(\\bi{r})$ and the zeros of its normal derivative across the curve. Theintersection points form a discrete random process which is the object of thisstudy. The field probability distribution function is completely specified bythe correlation $G(|\\bi{r}-\\bi{r}'|) = <\\Psi(\\bi{r}) \\Psi(\\bi{r}')>$.  Given an arbitrary $G(|\\bi{r}-\\bi{r}'|)$, we compute the two pointcorrelation function of the point process on the line, and derive otherstatistical measures (repulsion, rigidity) which characterize the short andlong range correlations of the intersection points. We use these statisticalmeasures to quantitatively characterize the complex patterns displayed byvarious kinds of nodal networks. We apply these statistics in particular tonodal patterns of random waves and of eigenfunctions of chaotic billiards. Ofspecial interest is the observation that for monochromatic random waves, thenumber variance of the intersections with long straight segments grows like $L\\ln L$, as opposed to the linear growth predicted by the percolation model,which was successfully used to predict other long range nodal properties ofthat field.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "I apply a two-step density-matrix renormalization group method to theanisotropic two-dimensional Hubbard model. As a prelude to this study, Icompare the numerical results to the exact one for the tight-binding model. Ifind a ground-state energy which agrees with the exact value up to four digitsfor systems as large as $24 \\times 25$. I then apply the method to theinteracting case. I find that for strong Hubbard interaction, the ground-stateis dominated by magnetic correlations.  These correlations are robust even in the presence of strong frustration.Interchain pair tunneling is negligible in the singlet and triplet channels andit is not enhanced by frustration. For weak Hubbard couplings, interchainnon-local singlet pair tunneling is enhanced and magnetic correlations arestrongly reduced. This suggests a possible superconductive ground state.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "NGC 7679 is a nearby luminous infrared Sy2 galaxy in which starburst and AGNactivities co-exist. The ionization structure is maintained by both the AGNpower-law continuum and starburst. The galaxy is a bright X-ray sourcepossessing a low X-ray column density N_H < 4 x 10^20 cm^{-2}. The Compton-thinnature of such unabsorbed objects infers that the simple formulation of theUnified model for SyGs is not applicable in their case. The main goal of thisarticle is to investigate both gas distribution and ionization structure in thecircumnuclear region of NGC 7679 in search for the presence of a hidden Sy1nucleus, using the [O III] 5007 luminosity as a tracer of AGN activity. The [OIII] 5007 image of the NGC 7679 shows elliptical isophotes extended along thePA ~ 80 deg in the direction to the counterpart galaxy NGC 7682. The maximum ofionization by the AGN power-law continuum traced by [O III] 5007/Halpha ratiois displaced by ~ 13 arcsec eastward from the nucleus. We conclude that thedust and gas in the high ionization direction has a direct view to the centralAGN engine. This possibly results in dust/star-formation decay. A largefraction of the unabsorbed Compton-thin Sy2s with [O III] luminosity > 10^41erg s^{-1} possesses a hidden AGN source (abridged).", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Based on our sample of 10095 galaxies with bulge-disc decompositions wederive the empirical B-band internal attenuation--inclination relation forgalaxy discs and their associated central bulges. Our results agree well withthe independently derived dust models of Tuffs et al., leading to a directconstraint on the mean opacity of spiral discs of Tau_B^f = 3.8 +/- 0.7(central face-on B-band opacity). Depending on inclination, the B-bandattenuation correction varies from 0.2 -- 1.1 mag for discs and from 0.8 -- 2.6mag for bulges. We find that, overall, 37 per cent of all B-band photonsproduced in discs in the nearby universe are absorbed by dust, a figure thatrises to 71 per cent for bulge photons. The severity of internal dustextinction is such that one must incorporate internal dust corrections in alloptical studies of large galaxy samples. This is particularly pertinent foroptical HST comparative evolutionary studies as the dust properties will alsobe evolving. We use the new results to revise our recent estimates of thespheroid and disc luminosity functions. From our best fitting dust models wederive a redshift zero cosmic dust density of rho_{dust} ~ (5.3 +/- 1.7) x10^5, h M_{odot} Mpc^-3. This implies that (0.0083 +/- 0.0027), h per cent ofthe baryons in the Universe are in the form of dust and (11.9 +/- 1.7), h percent (Salpeter-`lite' IMF) are in the form of stars (~58 per cent reside ingalaxy discs, ~10 per cent in red elliptical galaxies, ~29 per cent inclassical galaxy bulges and the remainder in low luminosity blue spheroidsystems/components). [Abridged]", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Recent observations have demonstrated a significant growth in the integratedstellar mass of the red sequence since z=1, dominated by a steadily increasingnumber of galaxies with stellar masses M* < 10^11 M_sun. In this paper, we usethe COMBO-17 photometric redshift survey in conjunction with deep Spitzer 24micron data to explore the relationship between star formation and the growthof stellar mass. We calculate `star formation rate functions' in four differentredshift slices, splitting also into contributions from the red sequence andblue cloud for the first time. We find that the growth of stellar mass sincez=1 is consistent with the integrated star formation rate. Yet, most of thestars formed are in blue cloud galaxies. If the stellar mass already in, andformed in, z<1 blue cloud galaxies were to stay in the blue cloud the totalstellar mass in blue galaxies would be dramatically overproduced. We explorethe expected evolution of stellar mass functions, finding that in this picturethe number of massive M* > 3x10^10 M_sun blue galaxies would also beoverproduced; i.e., most of the new stars formed in blue cloud galaxies are inthe massive galaxies. We explore a simple truncation scenario in which these`extra' blue galaxies have their star formation suppressed by an unspecifiedmechanism or mechanisms; simple cessation of star formation in these extra bluegalaxies is approximately sufficient to build up the red sequence at M*<10^11M_sun.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "A non-Hermitian complex symmetric 2x2 matrix toy model is used to studyprojective Hilbert space structures in the vicinity of exceptional points(EPs). The bi-orthogonal eigenvectors of a diagonalizable matrix arePuiseux-expanded in terms of the root vectors at the EP. It is shown that theapparent contradiction between the two incompatible normalization conditionswith finite and singular behavior in the EP-limit can be resolved byprojectively extending the original Hilbert space. The complementarynormalization conditions correspond then to two different affine charts of thisenlarged projective Hilbert space. Geometric phase and phase jump behavior areanalyzed and the usefulness of the phase rigidity as measure for the distanceto EP configurations is demonstrated. Finally, EP-related aspects ofPT-symmetrically extended Quantum Mechanics are discussed and a conjectureconcerning the quantum brachistochrone problem is formulated.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We have analyzed the HI aperture synthesis image of the Large MagellanicCloud (LMC), using an objective and quantitative measure of topology tounderstand the HI distribution hosting a number of holes and clumps of varioussizes in the medium. The HI distribution shows different topology at fourdifferent chosen scales. At the smallest scales explored (19-29 pc), the HImass is distributed in such a way that numerous clumps are embedded on top of alow density background. At the larger scales from 73 to 194 pc, it shows ageneric hole topology. These holes might have been formed mainly by stellarwinds from hot stars. At the scales from 240 to 340 pc, slightly above the diskscale-height of the gaseous disk, major clumps in the HI map change thedistribution to have a slight clump topology. These clumps include the giantcloud associations in the spiral arms and the thick filaments surroundingsuperholes. At the largest scales studied (390-485 pc), the hole topology ispresent again. Responsible to the hole topology at this scale are a fewsuperholes which seem mainly associated with supernova explosions in the outerdisk. The gaps between the bar and spiral arms have a minor effect on thetopology at this scale.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Let L be an ample holomorphic line bundle over a compact complex Hermitianmanifold X. Any fixed smooth Hermitian metric on L induces a Hilbert spacestructure on the space of global holomorphic sections with values in the k:thtensor power of L. In this paper various convergence results are obtained forthe corresponding Bergman kernels. The convergence is studied in the large klimit and is expressed in terms of the equilibrium metric associated to thefixed metric, as well as in terms of the Monge-Ampere measure of the fixedmetric itself on a certain support set. It is also shown that the equilibriummetric has Lipschitz continuous first derivatives. These results can be seen asgeneralizations of well-known results concerning the case when the curvature ofthe fixed metric is positive (the corresponding equilibrium metric is thensimply the fixed metric itself).", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We study 7 Gamma Ray Bursts (GRBs), detected both by the BATSE instrument,on-board the Compton Gamma Ray Observatory, and by the Wide Field Camera (WFC),on-board BeppoSAX. These bursts have measured spectroscopic redshifts and are asizeable fraction of the bursts defining the correlation between the peakenergy E_peak (i.e. the peak of the vFv spectrum) and the total promptisotropic energy E_iso (the so called \"Amati\" relation). Recent theoreticalinterpretations of this correlation assume that black-body emission dominatesthe time resolved spectra of GRBs, even if, in the time integrated spectrum,its presence may be hidden by the change of its temperature and by the dilutionof a possible non-thermal power law component. We perform a time resolvedspectral analysis, and show that the sum of a power-law and a black-body givesacceptable fits to the time dependent spectra within the BATSE energy range,but overpredicts the flux in the WFC X-ray range. Moreover, a fit with a cutoffpower-law plus a black-body is consistent with the WFC data, but the black-bodycomponent contributes a negligible fraction of the total flux. On the contrary,we find that fitting the spectra with a Band model or a simple cutoff power-lawmodel yields an X-ray flux and spectral slope which well matches the WFCspectra.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "A concentration graph associated with a random vector is an undirected graphwhere each vertex corresponds to one random variable in the vector. The absenceof an edge between any pair of vertices (or variables) is equivalent to fullconditional independence between these two variables given all the othervariables. In the multivariate Gaussian case, the absence of an edgecorresponds to a zero coefficient in the precision matrix, which is the inverseof the covariance matrix. It is well known that this concentration graphrepresents some of the conditional independencies in the distribution of theassociated random vector. These conditional independencies correspond to the\"separations\" or absence of edges in that graph. In this paper we assume thatthere are no other independencies present in the probability distribution thanthose represented by the graph. This property is called the perfectMarkovianity of the probability distribution with respect to the associatedconcentration graph. We prove in this paper that this particular concentrationgraph, the one associated with a perfect Markov distribution, can be determinedby only conditioning on a limited number of variables. We demonstrate that thisnumber is equal to the maximum size of the minimal separators in theconcentration graph.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Mixed action lattice calculations allow for an additive lattice spacingdependent mass renormalization of mesons composed of one sea and one valencequark, regardless of the type of fermion discretization methods used in thevalence and sea sectors. The value of the mass renormalization depends upon thelattice actions used. This mixed meson mass shift is an important latticeartifact to determine for mixed action calculations; because it modifies thepion mass, it plays a central role in the low energy dynamics of all hadroniccorrelation functions. We determine the leading order, $\\mathcal{O}(a^2)$, andnext to leading order, $\\mathcal{O}(a^2 m_\\pi^2)$, additive mass shift of\\textit{valence-sea} mesons for a mixed lattice action with domain-wall valencefermions and rooted staggered sea fermions, relevant to the majority of currentlarge scale mixed action lattice efforts. We find that on the asqtad improvedcoarse MILC lattices, this additive mass shift is well parameterized in latticeunits by $\\Delta(am)^2 = 0.034(2) -0.06(2) (a m_\\pi)^2$, which in physicalunits, using $a=0.125$ fm, corresponds to $\\Delta(m)^2 = (291\\pm 8\\textrm{MeV})^2 -0.06(2) m_\\pi^2$. In terms of the mixed action effective fieldtheory parameters, the corresponding mass shift is given by $a^2\\Delta_\\mathrm{Mix} = (316 \\pm 4 \\textrm{MeV})^2$ at leading order plusnext-to-leading order corrections including the necessary chiral logarithms forthis mixed action calculation, determined in this work. Within the precision ofour calculation, one can not distinguish between the full next-to-leading ordereffective field theory analysis of this additive mixed meson mass shift and theparameterization given above.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "In a previous work (M. Campisi. Stud. Hist. Phil. M. P. 36 (2005) 275-290) wehave addressed the mechanical foundations of equilibrium thermodynamics on thebasis of the Generalized Helmholtz Theorem. It was found that the volumeentropy provides a good mechanical analogue of thermodynamic entropy because itsatisfies the heat theorem and it is an adiabatic invariant. This propertyexplains the ``equal'' sign in Clausius principle ($S_f \\geq S_i$) in a purelymechanical way and suggests that the volume entropy might explain the ``largerthan'' sign (i.e. the Law of Entropy Increase) if non adiabatic transformationswere considered. Based on the principles of microscopic (quantum or classical)mechanics here we prove that, provided the initial equilibrium satisfy thenatural condition of decreasing ordering of probabilities, the expectationvalue of the volume entropy cannot decrease for arbitrary transformationsperformed by some external sources of work on a insulated system. This can beregarded as a rigorous quantum mechanical proof of the Second Law. We discusshow this result relates to the Minimal Work Principle and improves overprevious attempts. The natural evolution of entropy is towards larger valuesbecause the natural state of matter is at positive temperature. Actually theLaw of Entropy Decrease holds in artificially prepared negative temperaturesystems.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We compare the use of galaxy asymmetry and pair proximity for measuringgalaxy merger fractions and rates for a volume limited sample of 3184 galaxieswith -21 < M(B) -5 log h < -18 mag. and 0.010 < z < 0.123 drawn from theMillennium Galaxy Catalogue. Our findings are that:  (i) Galaxies in close pairs are generally more asymmetric than isolatedgalaxies and the degree of asymmetry increases for closer pairs. At least 35%of close pairs (with projected separation of less than 20 h^{-1} kpc andvelocity difference of less than 500 km s^{-1}) show significant asymmetry andare therefore likely to be physically bound.  (ii) Among asymmetric galaxies, we find that at least 80% are eitherinteracting systems or merger remnants. However, a significant fraction ofgalaxies initially identified as asymmetric are contaminated by nearby stars orare fragmented by the source extraction algorithm. Merger rates calculated viaasymmetry indices need careful attention in order to remove the above sourcesof contamination, but are very reliable once this is carried out.  (iii) Close pairs and asymmetries represent two complementary methods ofmeasuring the merger rate. Galaxies in close pairs identify future mergers,occurring within the dynamical friction timescale, while asymmetries aresensitive to the immediate pre-merger phase and identify remnants.  (iv) The merger fraction derived via the close pair fraction and asymmetriesis about 2% for a merger rate of (5.2 +- 1.0) 10^{-4} h^3 Mpc^{-3} Gyr^{-1}.These results are marginally consistent with theoretical simulations (dependingon the merger time-scale), but imply a flat evolution of the merger rate withredshift up to z ~1.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "An interplanetary (IP) type-II-like radio burst is analyzed. It occurred on2003 June 17-18 in association with a fast halo coronal mass ejection (CME), anM6.8 soft-X-ray (SXR) flare, and produced a solar proton event. Unlike coronaltype II bursts and the ma jority of IP type II radio emissions, the IPtype-II-like event associated with the fast halo CME on June 17-18 variessmoothly in time and frequency and has a frequency bandwidth that is severaltimes larger than is typical for coronal and IP type II emissions. Moreover,the frequency change with time is inconsistent with that expected from plasmaradiation associated with a CME-driven shock. I suggest that this IPtype-II-like event, referred to here as an IP type II-S event, is not due toplasma radiation but, rather, incoherent synchrotron radiation fromnear-relativistic electrons entrained in the CME magnetic field, or in thesheath region between the shock and the CME driver. This event may be anexample of a new and distinct class of interplanetary radio phenomenon.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "A main distinguishing feature of a wireless network compared with a wirednetwork is its broadcast nature, in which the signal transmitted by a node mayreach several other nodes, and a node may receive signals from several othernodes simultaneously. Rather than a blessing, this feature is treated more asan interference-inducing nuisance in most wireless networks today (e.g., IEEE802.11). This paper shows that the concept of network coding can be applied atthe physical layer to turn the broadcast property into a capacity-boostingadvantage in wireless ad hoc networks. Specifically, we propose aphysical-layer network coding (PNC) scheme to coordinate transmissions amongnodes. In contrast to straightforward network coding which performs codingarithmetic on digital bit streams after they have been received, PNC makes useof the additive nature of simultaneously arriving electromagnetic (EM) wavesfor equivalent coding operation. And in doing so, PNC can potentially achieve100% and 50% throughput increases compared with traditional transmission andstraightforward network coding, respectively, in multi-hop networks. Morespecifically, the information-theoretic capacity of PNC is almost double thatof traditional transmission in the SNR region of practical interest (higherthan 0dB). We believe this is a first paper that ventures into EM-wave-basednetwork coding at the physical layer and demonstrates its potential forboosting network capacity.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The set of solutions of random constraint satisfaction problems (zero energygroundstates of mean-field diluted spin glasses) undergoes several structuralphase transitions as the amount of constraints is increased. This set firstbreaks down into a large number of well separated clusters. At the freezingtransition, which is in general distinct from the clustering one, somevariables (spins) take the same value in all solutions of a given cluster. Inthis paper we study the critical behavior around the freezing transition, whichappears in the unfrozen phase as the divergence of the sizes of therearrangements induced in response to the modification of a variable. Theformalism is developed on generic constraint satisfaction problems and appliedin particular to the random satisfiability of boolean formulas and to thecoloring of random graphs. The computation is first performed in random treeensembles, for which we underline a connection with percolation models and withthe reconstruction problem of information theory. The validity of these resultsfor the original random ensembles is then discussed in the framework of thecavity method.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We study the S=1/2 Heisenberg antiferromagnet on a square lattice withnearest-neighbor and plaquette four-spin exchanges (introduced by A.W. Sandvik,Phys. Rev. Lett. {\\bf 98}, 227202 (2007).)  This model undergoes a quantum phase transition from a spontaneouslydimerized phase to N\\'eel order at a critical coupling. We show that as thecritical point is approached from the dimerized side, the system exhibitsstrong fluctuations in the dimer background, reflected in the presence of alow-energy singlet mode, with a simultaneous rise in the triplet quasiparticledensity. We find that both singlet and triplet modes of high density condenseat the transition, signaling restoration of lattice symmetry. In our approach,which goes beyond mean-field theory in terms of the triplet excitations, thetransition appears sharp; however since our method breaks down near thecritical point, we argue that we cannot make a definite conclusion regardingthe order of the transition.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We study planar clusters consisting of loops including a Josephson$\\pi$-junction ($\\pi$-rings). Each $\\pi$-ring carries a persistent current andbehaves as a classical orbital moment. The type of particular state associatedwith the orientation of orbital moments at the cluster depends on theinteraction between these orbital moments and can be easily controlled, i.e. bya bias current or by other means. We show that these systems can be describedby the two-dimensional Ising model with competing nearest-neighbor and diagonalinteractions and investigate the phase diagram of this model. Thecharacteristic features of the model are analyzed based on the exact solutionsfor small clusters such as a 5-site square plaquette as well as on a mean-fieldtype approach for the infinite square lattice of Ising spins. The results arecompared with spin patterns obtained by Monte Carlo simulations for the 100$\\times$ 100 square lattice and with experiment. We show that the $\\pi$-ringclusters may be used as a new type of superconducting memory elements. Theobtained results may be verified in experiments and are applicable to adiabaticquantum computing where the states are switched adiabatically with the slowchange of coupling constants.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We obtained comprehensive sets of elemental abundances for eleven dampedLy-alpha systems (DLAs) at z_DLA=1.7-2.5. In Paper I of this series, we showedfor three DLA galaxies that we can derive their star formation histories andages from a detailed comparison of their intrinsic abundance patterns withchemical evolution models. We determine in this paper the star formationproperties of six additional DLA galaxies. The derived results confirm that nosingle star formation history explains the diverse sets of abundance patternsin DLAs. We demonstrate that the various star formation histories reproducingthe DLA abundance patterns are typical of local irregular, dwarf starburst andquiescent spiral galaxies. Independent of the star formation history, the DLAshave a common characteristic of being weak star forming galaxies; models withhigh star formation efficiencies are ruled out. All the derived DLA starformation rates per unit area are moderate or low, with values between -3.2 <log SFR < -1.1 M_sol yr^{-1} kpc^{-2}. The DLA abundance patterns require alarge spread in ages ranging from 20 Myr up to 3 Gyr. The oldest DLA in oursample is observed at z_DLA=1.864 with an age estimated to more than 3 Gyr; itnicely indicates that galaxies were already forming at z_f>10. But, most of theDLAs show ages much younger than that of the Universe at the epoch ofobservation. Young galaxies thus seem to populate the high redshift Universe atz>2, suggesting relatively low redshifts of formation (z~3) for mosthigh-redshift galaxies. The DLA star formation properties are compared withthose of other high-redshift galaxies identified in deep imaging surveys withthe aim of obtaining a global picture of high-redshift objects.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The Kripke semantics of classical propositional normal modal logic is madealgebraic via an embedding of Kripke structures into the larger class ofpointed stably supported quantales. This algebraic semantics subsumes thetraditional algebraic semantics based on lattices with unary operators, and itsuggests natural interpretations of modal logic, of possible interest in theapplications, in structures that arise in geometry and analysis, such asfoliated manifolds and operator algebras, via topological groupoids and inversesemigroups. We study completeness properties of the quantale based semanticsfor the systems K, T, K4, S4, and S5, in particular obtaining an axiomatizationfor S5 which does not use negation or the modal necessity operator. Asadditional examples we describe intuitionistic propositional modal logic, thelogic of programs PDL, and the ramified temporal logic CTL.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Two approaches for closing the turbulence subgrid-scale stress tensor interms of matrix exponentials are introduced and compared. The first approach isbased on a formal solution of the stress transport equation in which theproduction terms can be integrated exactly in terms of matrix exponentials.This formal solution of the subgrid-scale stress transport equation is shown tobe useful to explore special cases, such as the response to constant velocitygradient, but neglecting pressure-strain correlations and diffusion effects.The second approach is based on an Eulerian-Lagrangian change of variables,combined with the assumption of isotropy for the conditionally averagedLagrangian velocity gradient tensor and with the `Recent Fluid Deformation'(RFD) approximation. It is shown that both approaches lead to the same basicclosure in which the stress tensor is expressed as the product of the matrixexponential of the resolved velocity gradient tensor multiplied by itstranspose. Short-time expansions of the matrix exponentials are shown toprovide an eddy-viscosity term and particular quadratic terms, and thus allow areinterpretation of traditional eddy-viscosity and nonlinear stress closures.The basic feasibility of the matrix-exponential closure is illustrated byimplementing it successfully in Large Eddy Simulation of forced isotropicturbulence. The matrix-exponential closure employs the drastic approximation ofentirely omitting the pressure-strain correlation and other `nonlinearscrambling' terms. But unlike eddy-viscosity closures, the matrix exponentialapproach provides a simple and local closure that can be derived directly fromthe stress transport equation with the production term, and using physicallymotivated assumptions about Lagrangian decorrelation and upstream isotropy.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "In the canonical formalism of statistical physics, a signature of a firstorder phase transition for finite systems is the bimodal distribution of anorder parameter. Previous thermodynamical studies of nuclear sources producedin heavy-ion collisions provide information which support the existence of aphase transition in those finite nuclear systems. Some results suggest that theobservable Z1 (charge of the biggest fragment) can be considered as a reliableorder parameter of the transition. This talk will show how from peripheralcollisions studied with the INDRA detector at GSI we can obtain this bimodalbehaviour of Z1. Getting rid of the entrance channel effects and under theconstraint of an equiprobable distribution of excitation energy (E*), we usethe canonical description of a phase transition to link this bimodal behaviourwith the residual convexity of the entropy. Theoretical (with and without phasetransition) and experimental Z1-E* correlations are compared. This comparisonallows us to rule out the case without transition. Moreover that quantitativecomparison provides us with information about the coexistence region in theZ1-E* plane which is in good agreement with that obtained with the signal ofabnormal uctuations of configurational energy (microcanonical negative heatcapacity).", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The Method of Invariant Grid (MIG) is an iterative procedure for modelreduction in chemical kinetics which is based on the notion of Slow InvariantManifold (SIM) [1-4]. Important role, in that method, is played by the initialgrid which, once refined, gives a description of the invariant manifold: theinvariant grid. A convenient way to get a first approximation of the SIM isgiven by the Spectral Quasi Equilibrium Manifold (SQEM) [1-2]. In the presentpaper, a flexible numerical method to construct the discrete analog of a QuasiEquilibrium Manifold, in any dimension, is presented. That object is namedQuasi Equilibrium Grid (QEG), while the procedure Quasi Equilibrium GridAlgorithm. Extensions of the QEM notion are also suggested. The QEG is anumerical tool which can be used to find a grid-based approximation for thelocus of minima of a convex function under some linear constraints. The methodis validated by construction of one and two-dimensional grids for modelhydrogen oxidation reaction.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present a survey of mid-infrared gas-phase lines toward a sample of 76circumstellar disks around low mass pre-main sequence stars from the Spitzer\"Cores to Disks\" legacy program. We report the first detections of [Ne II] and[Fe I] toward classical T Tauri stars in ~20% respectively ~9% of our sources.The observed [Ne II] line fluxes and upper limits are consistent with [Ne II]excitation in an X-ray irradiated disk around stars with X-ray luminositiesL_X=10^{29}-10^{31} erg s^{-1}. [Fe I] is detected at ~10^-5-10^-4 L_Sun, butno [S I] or [Fe II] is detected down to ~10^{-6} L_Sun. The [Fe I] detectionsindicate the presence of gas-rich disks with masses of >~0.1 M_J. No H_2 0-0S(0) and S(1) disk emission is detected, except for S(1) toward one source.These data give upper limits on the warm (T~100-200K) gas mass of a few Jovianmasses, consistent with recent T Tauri disk models which include gas heating bystellar radiation. Compact disk emission of hot (T>~500K) gas is observedthrough the H_2 0-0 S(2) and/or S(3) lines toward ~8% of our sources. The linefluxes are, however, higher by more than an order of magnitude than thosepredicted by recent disk models, even when X-ray and excess UV radiation areincluded. Similarly the [Ne II]/H_2 0-0 S(2) ratios for these sources are lowerthan predicted, consistent with the presence of an additional hot molecular gascomponent not included in current disk models. Oblique shocks of stellar windsinteracting with the disk can explain many aspects of the hot gas emission, butare inconsistent with the non-detection of [S I] and [Fe II] lines.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The problem of limit shapes in the six-vertex model with domain wall boundaryconditions is addressed by considering a specially tailored bulk correlationfunction, the emptiness formation probability. A closed expression of thiscorrelation function is given, both in terms of certain determinant andmultiple integral, which allows for a systematic treatment of the limit shapesof the model for full range of values of vertex weights. Specifically, we showthat for vertex weights corresponding to the free-fermion line on the phasediagram, the emptiness formation probability is related to a one-matrix modelwith a triple logarithmic singularity, or Triple Penner model. The saddle-pointanalysis of this model leads to the Arctic Circle Theorem, and itsgeneralization to the Arctic Ellipses, known previously from domino tilings.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "In 1921 Blichfeldt gave an upper bound on the number of integral pointscontained in a convex body in terms of the volume of the body. More precisely,he showed that $#(K\\cap\\Z^n)\\leq n! \\vol(K)+n$, whenever $K\\subset\\R^n$ is aconvex body containing $n+1$ affinely independent integral points. Here weprove an analogous inequality with respect to the surface area $\\F(K)$, namely$ #(K\\cap\\Z^n) < \\vol(K) + ((\\sqrt{n}+1)/2) (n-1)! \\F(K)$. The proof is basedon a slight improvement of Blichfeldt's bound in the case when $K$ is anon-lattice translate of a lattice polytope, i.e., $K=t+P$, where$t\\in\\R^n\\setminus\\Z^n$ and $P$ is an $n$-dimensional polytope with integralvertices. Then we have $#((t+P)\\cap\\Z^n)\\leq n! \\vol(P)$.  Moreover, in the 3-dimensional case we prove a stronger inequality, namely$#(K\\cap\\Z^n) < \\vol(K) + 2 \\F(K)$.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The polarized neutron scattering in helimagnetic MnSi at low $T$ revealsexistence of a partially disordered chiral state at ambient pressure in themagnetic field applied along $<111>$ axis below the first order transition tothe non-chiral ferromagnetic state. This unexpected phenomenon is explained bythe analysis of the spin-wave spectrum. We demonstrate that the square of thespin-wave gap becomes negative under magnetic field applied along $<111>$ and$<110>$ but not along the $<100>$ direction. It is a result of competitionbetween the spin-wave interaction and cubic anisotropy. This negative signmeans an instability of the spin wave spectrum for the helix and leads to adestruction of the helical order, giving rise to the partially disordered statebelow the first order ferromagnetic transition.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present both numerical and analytical study of graphene roughness with acrystal structure including $500 \\times 500$ atoms. The roughness caneffectively result in a random gauge field and has important consequences forits electronic structure. Our results show that its height fluctuations insmall scales have scaling behavior with a temperature dependent roughnessexponent in the interval of $ 0.6 < \\chi < 0.7 $. The correlation function ofheight fluctuations depends upon temperature with characteristic length scaleof $ \\approx 90 {\\AA}$ (at room temperature). We show that the correlationfunction of the induced gauge field has a short-range nature with correlationlength of about $\\simeq 2-3 {\\AA}$. We also treat the problem analytically byusing the Martin-Siggia-Rose method. The renormalization group flows did notyield any delocalized-localized transition arising from the graphene roughness.Our results are in good agreement with recent experimental observations.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Pulse shape discrimination (PSD) is one of the most distinctive features ofliquid scintillators. Since the introduction of the scintillation techniques inthe field of particle detection, many studies have been carried out tocharacterize intrinsic properties of the most common liquid scintillatormixtures in this respect. Several application methods and algorithms able toachieve optimum discrimination performances have been developed. However, thevast majority of these studies have been performed on samples of smalldimensions. The Counting Test Facility, prototype of the solar neutrinoexperiment Borexino, as a 4 ton spherical scintillation detector immersed in1000 tons of shielding water, represents a unique opportunity to extend thesmall-sample PSD studies to a large-volume setup. Specifically, in this work weconsider two different liquid scintillation mixtures employed in CTF,illustrating for both the PSD characterization results obtained either with theprocessing of the scintillation waveform through the optimum Gatti's method, orvia a more conventional approach based on the charge content of thescintillation tail. The outcomes of this study, while interesting per se, arealso of paramount importance in view of the expected Borexino detectorperformances, where PSD will be an essential tool in the framework of thebackground rejection strategy needed to achieve the required sensitivity to thesolar neutrino signals.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We consider a list decoding algorithm recently proposed by Pellikaan-Wu\\cite{PW2005} for $q$-ary Reed-Muller codes $\\mathcal{RM}_q(\\ell, m, n)$ oflength $n \\leq q^m$ when $\\ell \\leq q$. A simple and easily accessiblecorrectness proof is given which shows that this algorithm achieves a relativeerror-correction radius of $\\tau \\leq (1 - \\sqrt{{\\ell q^{m-1}}/{n}})$. This isan improvement over the proof using one-point Algebraic-Geometric codes givenin \\cite{PW2005}. The described algorithm can be adapted to decodeProduct-Reed-Solomon codes.  We then propose a new low complexity recursive algebraic decoding algorithmfor Reed-Muller and Product-Reed-Solomon codes. Our algorithm achieves arelative error correction radius of $\\tau \\leq \\prod_{i=1}^m (1 -\\sqrt{k_i/q})$. This technique is then proved to outperform the Pellikaan-Wumethod in both complexity and error correction radius over a wide range of coderates.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The configurations of single and double bonds in polycyclic hydrocarbons areabstracted as Kekul\\'e states of graphs. Sending a so-called soliton over anopen channel between ports (external nodes) of the graph changes the Kekul\\'estate and therewith the set of open channels in the graph. This switchingbehaviour is proposed as a basis for molecular computation. The proposal ishighly speculative but may have tremendous impact.  Kekul\\'e states with the same boundary behaviour (port assignment) can beregarded as equivalent. This gives rise to the abstraction of Kekul\\'e cells.The basic theory of Kekul\\'e states and Kekul\\'e cells is developed here, up tothe classification of Kekul\\'e cells with $\\leq 4$ ports. To put the theory incontext, we generalize Kekul\\'e states to semi-Kekul\\'e states, which form thesolutions of a linear system of equations over the field of the bits 0 and 1.We briefly study so-called omniconjugated graphs, in which every portassignment of the right signature has a Kekul\\'e state. Omniconjugated graphsmay be useful as connectors between computational elements. We finallyinvestigate some examples with potentially useful switching behaviour.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We have compiled the largest sample of multiwavelength spectral energydistributions (SEDs) of Broad Absorption Line (BAL) quasars to date, from theradio to the X-ray. We present new Spitzer MIPS (24, 70, and 160 micron)observations of 38 BAL quasars in addition to data from the literature andpublic archives. In general, the mid-infrared properties of BAL quasars areconsistent with those of non-BAL quasars of comparable luminosity. Inparticular, the optical-to-mid-infrared luminosity ratios of the twopopulations are indistinguishable. We also measure or place upper limits on thecontribution of star formation to the far-infrared power. Of 22 (57%) upperlimits, seven quasars have sufficiently sensitive constraints to conclude thatstar formation likely contributes little (<20%) to their far-infrared power.The 17 BAL quasars (45%) with detected excess far-infrared emission likely hosthyperluminous starbursts with L_fir,SF=10^{13-14} L_sun. Mid-infrared throughX-ray composite BAL quasar SEDs are presented, incorporating all of theavailable photometry. Overall, we find no compelling evidence for inherentdifferences between the SEDs of BAL vs. non-BAL quasars of comparableluminosity. Therefore a ``cocoon'' picture of a typical BAL quasar outflowwhereby the wind covers a large fraction of the sky is not supported by themid-infrared SED comparison with normal quasars, and the disk-wind paradigmwith a typical radio-quiet quasar hosting a BAL region remains viable.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Presenting theoretical arguments and numerical results we demonstratelong-range intrachain correlations in concentrated solutions and melts of longflexible polymers which cause a systematic swelling of short chain segments.They can be traced back to the incompressibility of the melt leading to aneffective repulsion $u(s) \\approx s/\\rho R^3(s) \\approx ce/\\sqrt{s}$ whenconnecting two segments together where $s$ denotes the curvilinear length of asegment, $R(s)$ its typical size, $ce \\approx 1/\\rho be^3$ the ``swellingcoefficient\", $be$ the effective bond length and $\\rho$ the monomer density.The relative deviation of the segmental size distribution from the idealGaussian chain behavior is found to be proportional to $u(s)$. The analysis ofdifferent moments of this distribution allows for a precise determination ofthe effective bond length $be$ and the swelling coefficient $ce$ ofasymptotically long chains. At striking variance to the short-range decaysuggested by Flory's ideality hypothesis the bond-bond correlation function oftwo bonds separated by $s$ monomers along the chain is found to decayalgebraically as $1/s^{3/2}$. Effects of finite chain length are consideredbriefly.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "In this notes unbounded regular operators on Hilbert $C^*$-modules overarbitrary $C^*$-algebras are discussed. A densely defined operator $t$possesses an adjoint operator if the graph of $t$ is an orthogonal summand.Moreover, for a densely defined operator $t$ the graph of $t$ is orthogonallycomplemented and the range of $P_FP_{G(t)^\\bot}$ is dense in its biorthogonalcomplement if and only if $t$ is regular. For a given $C^*$-algebra $\\mathcalA$ any densely defined $\\mathcal A$-linear closed operator $t$ between Hilbert$C^*$-modules is regular, if and only if any densely defined $\\mathcalA$-linear closed operator $t$ between Hilbert $C^*$-modules admits a denselydefined adjoint operator, if and only if $\\mathcal A$ is a $C^*$-algebra ofcompact operators. Some further characterizations of closed and regular modularoperators are obtained.  Changes 1: Improved results, corrected misprints, added references. Acceptedby J. Operator Theory, August 2007 / Changes 2: Filled gap in the proof of Thm.3.1, changes in the formulations of Cor. 3.2 and Thm. 3.4, updated referencesand address of the second author.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present measurements of the mean dense core lifetimes in numericalsimulations of magnetically supercritical, turbulent, isothermal molecularclouds, in order to compare with observational determinations. \"Prestellar\"lifetimes (given as a function of the mean density within the cores, which inturn is determined by the density threshold n_thr used to define them) areconsistent with observationally reported values, ranging from a few to severalfree-fall times. We also present estimates of the fraction of cores in the\"prestellar\", \"stellar'', and \"failed\" (those cores that redisperse back intothe environment) stages as a function of n_thr. The number ratios are measuredindirectly in the simulations due to their resolution limitations. Our approachcontains one free parameter, the lifetime of a protostellar object t_yso (Class0 + Class I stages), which is outside the realm of the simulations. Assuming avalue t_yso = 0.46 Myr, we obtain number ratios of starless to stellar coresranging from 4-5 at n_thr = 1.5 x 10^4 cm^-3 to 1 at n_thr = 1.2 x 10^5 cm^-3,again in good agreement with observational determinations. We also find thatthe mass in the failed cores is comparable to that in stellar cores at n_thr =1.5 x 10^4 cm^-3, but becomes negligible at n_thr = 1.2 x 10^5 cm^-3, inagreement with recent observational suggestions that at the latter densitiesthe cores are in general gravitationally dominated. We conclude by noting thatthe timescale for core contraction and collapse is virtually the same in thesubcritical, ambipolar diffusion-mediated model of star formation, in the modelof star formation in turbulent supercritical clouds, and in a modelintermediate between the previous two, for currently accepted values of theclouds' magnetic criticality.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Coherent Harmonic Generation (CHG), and in particular Nonlinear HarmonicGeneration (NHG), is of importance for both short wavelength Free-ElectronLasers (FELs), in relation with the achievement of shorter wavelengths with afixed electron-beam energy, and high-average power FEL resonators, in relationwith destructive effects of higher harmonics radiation on mirrors. In thispaper we present a treatment of NHG from helical wigglers with particularemphasis on the second harmonic. Our study is based on an exact analyticalsolution of Maxwell's equations, derived with the help of a Green's functionmethod. In particular, we demonstrate that nonlinear harmonic generation (NHG)from helical wigglers vanishes on axis. Our conclusion is in open contrast withresults in literature, that include a kinematical mistake in the description ofthe electron motion.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "In the previous paper, based on the $SU(2)_{f}\\times SU(2)_{s}$ heavy quarksymmetries of the QCD Lagrangian in the heavy quark limit, the Bethe-Salpeterequation for the heavy baryon $\\Lambda_b$ was established with the picture that$\\Lambda_b$ is composed of a heavy quark and a scalar light diquark. In thepresent work, we apply this model to calculate $\\mu_\\pi^2$ for $\\Lambda_b$, theaverage kinetic energy of the heavy quark inside $\\Lambda_{b}$. This quantityis particularly interesting since it can be measured in experiments and sinceit contributes to the inclusive semileptonic decays of $\\Lambda_b$ whencontributions from higher order terms in $1/M_b$ expansions are taken intoaccount and consequently influences the determination of theCabibbo-Kobayashi-Maskawa matrix elements $V_{ub}$ and $V_{cb}$. We find that$\\mu_\\pi^2$ for $\\Lambda_b$ is $0.25GeV^2$ $\\sim$ $0.95GeV^2$, depending on theparameters in the model including the light diquark mass and the interactionstrength between the heavy quark and the light diquark in the kernel of the BSequation. We also find that this result is consistent with the value of$\\mu_\\pi^2$ for $\\Lambda_b$ which is derived from the experimental value of$\\mu_\\pi^2$ for the $B$ meson with the aid of the heavy quark effective theory.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We study stellar configurations and the space-time around them in metric$f(R)$ theories of gravity. In particular, we focus on the polytropic model ofthe Sun in the $f(R)=R-\\mu^4/R$ model. We show how the stellar configuration inthe $f(R)$ theory can, by appropriate initial conditions, be selected to beequal to that described by the Lane-Emden -equation and how a simple scalingrelation exists between the solutions. We also derive the correct solutionanalytically near the center of the star in $f(R)$ theory. Previous analyticaland numerical results are confirmed, indicating that the space-time around theSun is incompatible with Solar System constraints on the properties of gravity.Numerical work shows that stellar configurations, with a regular metric at thecenter, lead to $\\gamma_{PPN}\\simeq1/2$ outside the star ie. theSchwarzschild-de Sitter -space-time is not the correct vacuum solution for suchconfigurations. Conversely, by selecting the Schwarzschild-de Sitter -metric asthe outside solution, we find that the stellar configuration is unchanged butthe metric is irregular at the center. The possibility of constructing a $f(R)$theory compatible with the Solar System experiments and possible newconstraints arising from the radius-mass -relation of stellar objects isdiscussed.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Competitive random sequential adsorption on a line from a binary mix ofincident particles is studied using both an analytic recursive approach andMonte Carlo simulations. We find a strong correlation between the small and thelarge particle distributions so that while both partial contributions to thefill factor fluctuate widely, the variance of the total fill factor remainsrelatively small. The variances of partial contributions themselves are quitedifferent between the smaller and the larger particles, with the largerparticle distribution being more correlated. The disparity in fluctuations ofpartial fill factors increases with the particle size ratio. The additionalvariance in the partial contribution of smaller particle originates from thefluctuations in the size of gaps between larger particles. We discuss theimplications of our results to semiconductor high-energy gamma detectors wherethe detector energy resolution is controlled by correlations in the cascadeenergy branching process.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We determine the contribution of stars in galaxies, intracluster stars, andthe intracluster medium to the total baryon budget in nearby galaxy clustersand groups. We find that the baryon mass fraction (f_b) within r500 is constantfor systems with M500 between 6e13 and 1e15 Msun. Although f_b is lower thanthe WMAP value, the shortfall is on the order of both the observationalsystematic uncertainties and the depletion of baryons within r500 that ispredicted by simulations. The data therefore provide no compelling evidence forundetected baryonic components, particularly any that vary in importance withcluster mass. A unique feature of the current analysis is direct inclusion ofthe contribution of intracluster light (ICL) in the baryon budget. The increasein X-ray gas mass fraction with increasing total mass is entirely accounted forby a decrease in the total stellar mass fraction, supporting the argument thatthe behavior of both the stellar and X-ray gas components is dominated by adecrease in star formation efficiency in more massive environments. Within justthe stellar component, the fraction of the total stellar luminosity in the BCGand ICL decreases as velocity dispersion increases, suggesting that the BCG+ICLcomponent, and in particular the dominant ICL component, grows less efficientlyin higher mass environments. The degree to which this behavior arises from oursample selection, which favored systems with central, giant ellipticalgalaxies, remains unclear. A more robust result is the identification of lowmass groups with large BCG+ICL components, demonstrating that the creation ofintracluster stars does not require a massive cluster environment. Within r500and r200, the BCG+ICL contributes on average 40% and 33% of the total stellarlight, respectively.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The observed apparent velocities and luminosities of the relativistic jets inAGNs are significantly different from their intrinsic values due to strongspecial relativistic effects. We adopt the maximum likelihood method todetermine simultaneously the intrinsic luminosity function and the Lorentzfactor distribution of a sample of AGNs. The values of the best estimatedparameters are consistent with the previous results, but with much betteraccuracy. In previous study, it was assumed that the shape of the observedluminosity function of Fanaroff-Riley type II radio galaxies is the same withthe intrinsic luminosity function of radio loud quasars. Our results prove thevalidity of this assumption. We also find that low and high redshift groupsdivided by z=0.1 are likely to be from different parent populations.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Let G be a simple and simply-connected complex algebraic group, P \\subset G aparabolic subgroup. We prove an unpublished result of D. Peterson which statesthat the quantum cohomology QH^*(G/P) of a flag variety is, up to localization,a quotient of the homology H_*(Gr_G) of the affine Grassmannian \\Gr_G of G. Asa consequence, all three-point genus zero Gromov-Witten invariants of $G/P$ areidentified with homology Schubert structure constants of H_*(Gr_G),establishing the equivalence of the quantum and homology affine Schubertcalculi.  For the case G = B, we use the Mihalcea's equivariant quantum Chevalleyformula for QH^*(G/B), together with relationships between the quantum Bruhatgraph of Brenti, Fomin and Postnikov and the Bruhat order on the affine Weylgroup. As byproducts we obtain formulae for affine Schubert homology classes interms of quantum Schubert polynomials. We give some applications in quantumcohomology.  Our main results extend to the torus-equivariant setting.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We theoretically discuss how to tune the competition between Forster transferand spontaneous emission in a continuous and nondestructive fashion. Theproposed approach is especially suitable for delicate biological systems likelight harvesting complexes and fluorescent protein oligomers. We demonstratethat the manipulation of the density of photonic states at the emissionfrequency of the energy donor results in a change of the quantum efficienciesof the competing energy transfer and spontaneous emission processes. Thischange will be manifested in a modification of the donor and acceptor emissionintensities. Thus, by controlling the local density of photonic states Forstercoupled systems can be manipulated and analyzed without the need to physicallyseparate donor and acceptor chromophores for individual analysis, which is ofinterest, for example, for oligomeric reef coral fluorescent proteins.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "A new system, consisting of a double channel Fabry Perot etalon and laserdiodes emitting around 780 nm is described and proposed to be used for airrefractive index measurements. The principle of this refractometer is based onfrequency measurements between optical laser sources. It permitsquasi-instantaneous measurement with a resolution better than and uncertaintyin the range. Some preliminary results on the stability of this system and themeasurements of the refractive index of air with this apparatus are presented.The first measurements of the index of air at 780 nm are, within anexperimental uncertainty of the order of, in agreement with the predictedvalues by the so-called revised Edl\\'en equations. This result is to the bestof our knowledge the first to extend to the near infra-red the validity of therevised Edl\\'en equation derived for the wavelength range 350- 650 nm.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "[ABRIDGED] We recently presented evidence of a connection between thebrightness profiles of nearby early-type galaxies and the properties of the AGNthey host. The radio loudness of the AGN appears to be univocally related tothe host's brightness profile: radio-loud nuclei are only hosted by ``core''galaxies while radio-quiet AGN are only found in ``power-law'' galaxies. Weextend our analysis here to a sample of 42 nearby (V < 7000 km/s) Seyfertgalaxies hosted by early-type galaxies. We used the available HST images tostudy their brightness profiles. Having excluded complex and highly nucleatedgalaxies, in the remaining 16 objects the brightness profiles can besuccessfully modeled with a Nuker law with a steep nuclear cusp characteristicof ``power-law'' galaxies (with logarithmic slope 0.51 - 1.07). This result iswhat is expected for these radio-quiet AGN based on our previous findings, thusextending the validity of the connection between brightness profile and radioloudness to AGN of a far higher luminosity. We explored the robustness of thisresult against a different choice of the analytic form for the brightnessprofiles, using a Sersic law. In no object could we find evidence of a centrallight deficit with respect to a pure Sersic model, the defining feature of``core'' galaxies in this modeling framework. We conclude that, regardless ofthe modeling strategy, the dichotomy of AGN radio loudness can be univocallyrelated to the host's brightness profile. Our general results can be re-phrasedas ``radio-loud nuclei are hosted by core galaxies, while radio-quiet AGN arefound in non-core galaxies''.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We consider a model of socially interacting individuals that make a binarychoice in a context of positive additive endogenous externalities. Itencompasses as particular cases several models from the sociology and economicsliterature. We extend previous results to the case of a general distribution ofidiosyncratic preferences, called here Idiosyncratic Willingnesses to Pay(IWP). Positive additive externalities yield a family of inverse demand curvesthat include the classical downward sloping ones but also new ones with nonconstant convexity. When j, the ratio of the social influence strength to thestandard deviation of the IWP distribution, is small enough, the inverse demandis a classical monotonic (decreasing) function of the adoption rate. Even ifthe IWP distribution is mono-modal, there is a critical value of j above whichthe inverse demand is non monotonic, decreasing for small and high adoptionrates, but increasing within some intermediate range. Depending on the pricethere are thus either one or two equilibria. Beyond this first result, weexhibit the generic properties of the boundaries limiting the regions where thesystem presents different types of equilibria (unique or multiple). Theseproperties are shown to depend only on qualitative features of the IWPdistribution: modality (number of maxima), smoothness and type of support(compact or infinite). The main results are summarized as phase diagrams in thespace of the model parameters, on which the regions of multiple equilibria areprecisely delimited.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Solar prominences and filaments (prominences projected against the solardisk) exhibit a large variety of fine structures which are well observed downto the resolution limit of ground-based telescopes. We describe themorphological aspects of these fine structures which basically depend on thetype of a prominence (quiescent or active-region). Then we review currenttheoretical scenarios which are aimed at explaining the nature of thesestructures. In particular we discuss in detail the relative roles of magneticpressure and gas pressure (i.e., the value of the plasma-beta), as well as thedynamical aspects of the fine structures. Special attention is paid to recentnumerical simulations which include a complex magnetic topology, energy balance(heating and cooling processes), as well as the multidimensional radiativetransfer. Finally, we also show how new ground-based and space observations canreveal various physical aspects of the fine structures including theirprominence-corona transition regions in relation to the orientation of themagnetic field.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "It is widely believed that the perovskite Sr$_2$RuO$_4$ is an unconventionalsuperconductor with broken time reversal symmetry. It has been predicted thatsuperconductors with broken time reversal symmetry should have spontaneouslygenerated supercurrents at edges and domain walls. We have done careful imagingof the magnetic fields above Sr$_2$RuO$_4$ single crystals using scanning Hallbar and SQUID microscopies, and see no evidence for such spontaneouslygenerated supercurrents. We use the results from our magnetic imaging to placeupper limits on the spontaneously generated supercurrents at edges and domainwalls as a function of domain size. For a single domain, this upper limit isbelow the predicted signal by two orders of magnitude. We speculate on thecauses and implications of the lack of large spontaneous supercurrents in thisvery interesting superconducting system.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The observed association of Long Gamma-Ray Bursts (LGRBs) with peculiar TypeIc supernovae gives support to Woosley`s collapsar/hypernova model, in whichthe GRB is produced by the collapse of the rapidly rotating core of a massivestar to a black hole. The association of LGRBs with small star-forming galaxiessuggests low-metallicity to be a condition for a massive star to evolve to thecollapsar stage. Both completely-mixed single star models and binary starmodels are possible. In binary models the progenitor of the GRB is a massivehelium star with a close companion. We find that tidal synchronization duringcore-helium burning is reached on a short timescale (less than a fewmillennia). However, the strong core-envelope coupling in the subsequentevolutionary stages is likely to rule out helium stars with main-sequencecompanions as progenitors of hypernovae/GRBs. On the other hand, helium starsin close binaries with a neutron-star or black-hole companion can, despite thestrong core-envelope coupling in the post-helium burning phase, retainsufficient core angular momentum to produce a hypernova/GRB.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Context. Swift data are revolutionising our understanding of Gamma RayBursts. Since bursts fade rapidly, it is desirable to create and disseminateaccurate light curves rapidly.  Aims. To provide the community with an online repository of X-ray lightcurves obtained with Swift. The light curves should be of the quality expectedof published data, but automatically created and updated so as to beself-consistent and rapidly available. Methods. We have produced a suite ofprograms which automatically generates Swift/XRT light curves of GRBs. Effectsof the damage to the CCD, automatic readout-mode switching and pile-up areappropriately handled, and the data are binned with variable bin durations, asnecessary for a fading source.  Results. The light curve repository website(http://www.swift.ac.uk/xrt_curves) contains light curves, hardness ratios anddeep images for every GRB which Swift's XRT has observed. When new GRBs aredetected, light curves are created and updated within minutes of the dataarriving at the UK Swift Science Data Centre.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present the analysis and results of a 20 ks XMM-Newton observation ofRBS1423. X-ray spectral analysis is used to establish a significantly broadenedrelativistic iron K-alpha line from a highly ionised disk. A QSO at z=2.262 wasconsidered to be the optical counterpart of this ROSAT Bright Survey X-raysource. Based on the improved XMM-Newton source position we identified az=0.208 QSO as optical counterpart to RBS1423. The 0.2-12 keV X-ray luminosityof this radio-quiet QSO is 6x10^{44} erg/s. The XMM-EPIC spectra are welldescribed by a power law with a significantly broadened iron K-alpha line. Diskline models for both Schwarzschild and Kerr black holes require hydrogen-likeiron ions to fit the measured line profile. Significant ionisation of thereflection disk is confirmed by model fits with ionised disk models, resultingin an ionisation parameter xi~2000.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The Seyfert 2 galaxies NGC 2992 and NGC 3081 have been observed by INTEGRALand Swift. We report about the results and the comparison of the spectrum above10 keV based on INTEGRAL IBIS/ISGRI, Swift/BAT, and BeppoSAX/PDS. A spectrumcan be extracted in the X-ray energy band ranging from 1 keV up to 200 keV.Although NGC 2992 shows a complex spectrum below 10 keV, the hard tail observedby various missions exhibits a slope with photon index = 2, independent on theflux level during the observation. No cut-off is detectable up to the detectionlimit around 200 keV. In addition, NGC 3081 is detected in the INTEGRAL andSwift observation and also shows an unbroken Gamma = 1.8 spectrum up to 150keV. These two Seyfert galaxies give further evidence that a high-energycut-off in the hard X-ray spectra is often located at energies E_C >> 100 keV.In NGC 2992 a constant spectral shape is observed over a hard X-ray luminosityvariation by a factor of 11. This might indicate that the physical conditionsof the emitting hot plasma are constant, while the amount of plasma varies, dueto long-term flaring activity.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "There are nine metal-deficient stars that have Li abundances well below theLi plateau that is defined by over 100 unevolved stars with temperatures above5800 K and values of [Fe/H] $<$ $-$1.0. Abundances of Be have been determinedfor most of these ultra-Li-deficient stars in order to investigate the cause ofthe Li deficiencies. High-resolution and high signal-to-noise spectra have beenobtained in the Be II spectral region near 3130 \\AA for six ultra-Li-deficientstars with the Keck I telescope and its new uv-sensitive CCD on the upgradedHIRES. The spectrum synthesis technique has been used to determine Beabundances. All six stars are found to have Be deficiencies also. Two havemeasurable - but reduced - Be and four have only upper limits on Be. Theseresults are consistent with the idea that these Li- and Be-deficient stars areanalogous to blue stragglers. The stars have undergone mass transfer events (ormergers) which destroy or dilute both Li and Be. The findings cannot be matchedby the models that predict that the deficiencies are due to extra-mixing in asubset of halo stars that were initially rapid rotators, with the possibleexception of one star, G 139-8. Because the ultra-Li-deficient stars are alsoBe-deficient, they appear to be genuine outliers in population of halo starsused to determine the value of primordial Li; they no longer have the Li intheir atmospheres that was produced in the Big Bang.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present results of the HST Advanced Camera for Surveys spectroscopicground-based redshift survey in the field of A1689. We measure 98 redshifts,increasing the number of spectroscopically confirmed objects by sixfold. Wepresent two spectra from this catalog of the Sextet Arcs, images which arisefrom a strongly-lensed Lyman Break Galaxy (LBG) at a redshift of z=3.038.Gravitational lensing by the cluster magnifies its flux by a factor of ~16 andproduces six separate images with a total r-band magnitude of r_625=21.7. Thetwo spectra, each of which represents emission from different regions of theLBG, show H I and interstellar metal absorption lines at the systemic redshift.Significant variations are seen in Ly-alpha profile across a single galaxy,ranging from strong absorption to a combination of emission plus absorption. Aspectrum of a third image close to the brightest arc shows Ly-alpha emission atthe same redshift as the LBG, arising from either another spatially distinctregion of the galaxy, or from a companion galaxy close to the LBG. Taken as agroup, the Ly-alpha equivalent width in these three spectra decreases withincreasing equivalent width of the strongest interstellar absorption lines. Wediscuss how these variations can be used to understand the physical conditionsin the LBG. Intrinsically, this LBG is faint, ~0.1L*, and forming stars at amodest rate, ~4 solar masses per year. We also detect absorption line systemstoward the Sextet Arcs at z=2.873 and z=2.534. The latter system is seen acrosstwo of our spectra.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Bars in galaxies are mainly supported by particles trapped around stableperiodic orbits. These orbits represent oscillatory motion with only onefrequency, which is the bar driving frequency, and miss free oscillations. Weshow that a similar situation takes place in double bars: particles get trappedaround parent orbits, which in this case represent oscillatory motion with twofrequencies of driving by the two bars, and which also lack free oscillations.Thus the parent orbits, which constitute the backbone of an oscillatingpotential of two independently rotating bars, are the double-frequency orbits.These orbits do not close in any reference frame, but they map onto loops,first introduced by Maciejewski & Sparke (1997). Trajectories trapped aroundthe parent double-frequency orbit map onto a set of points confined within aring surrounding the loop.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We study the propagation of nucleons and nuclei in tissue-like media within aMonte Carlo Model for Heavy-ion Therapy (MCHIT) based on the GEANT4 toolkit(version 8.2). The model takes into account fragmentation of projectile nucleiand secondary interactions of produced nuclear fragments. Model predictions arevalidated with available experimental data obtained for water and PMMA phantomsirradiated by monoenergetic carbon-ion beams. The MCHIT model describes well(1) the depth-dose distributions in water and PMMA, (2) the doses measured forfragments of certain charge, (3) the distributions of positron emitting nuclearfragments produced by carbon-ion beams, and (4) the energy spectra of secondaryneutrons measured at different angles to the beam direction. Radial doseprofiles for primary nuclei and for different projectile fragments arecalculated and discussed as possible input for evaluation of biological dosedistributions. It is shown that at the periphery of the transverse dose profileclose to the Bragg peak the dose from secondary nuclear fragments is comparableto the dose from primary nuclei.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We use Monte-Carlo simulations to study aging phenomena and the occurence ofspinglass phases in systems of single-domain ferromagnetic nanoparticles underthe combined influence of dipolar interaction and anisotropy energy, fordifferent combinations of positional and orientational disorder. We find thatthe magnetic moments oriente themselves preferably parallel to their anisotropyaxes and changes of the total magnetization are solely achieved by 180 degreeflips of the magnetic moments, as in Ising systems. Since the dipolarinteraction favorizes the formation of antiparallel chain-like structures,antiparallel chain-like patterns are frozen in at low temperatures, leading toaging phenomena characteristic for spin-glasses. Contrary to the intuition,these aging effects are more pronounced in ordered than in disorderedstructures.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "A complete model of helium-like line and continuum emission has beenincorporated into the plasma simulation code Cloudy. All elements between Heand Zn are treated, any number of levels can be considered, and radiative andcollisional processes are included. This includes photoionization from alllevels, line transfer including continuum pumping and destruction by backgroundopacities, scattering, and collisional processes. The model is calculatedself-consistently along with the ionization and thermal structure of thesurrounding nebula. The result is a complete line and continuum spectrum of theplasma. Here we focus on the ions of the He I sequence and reconsider thestandard helium-like X-ray diagnostics. We first consider semi-analyticalpredictions and compare these with previous work in the low-density,optically-thin limit. We then perform numerical calculations of helium-likeX-ray emission (such as is observed in some regions of Seyferts) and predictline ratios as a function of ionizing flux, hydrogen density, and columndensity. In particular, we demonstrate that, in photoionized plasmas, the$R$-ratio, a density indicator in a collisional plasma, depends on theionization fraction and is strongly affected by optical depth for large columndensities. We also introduce the notion that the $R$-ratio is a measure of theincident continuum at UV wavelengths. The $G$-ratio, which istemperature-sensitive in a collisional plasma, is also discussed, and shown tobe strongly affected by continuum pumping and optical depth as well. Thesedistinguish a photoionized plasma from the more commonly studied collisionalcase.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We discuss the time evolution and matter-wave interference of Fermicondensates on the BEC side of Feshbach resonances for s and p-wavesuperfluids, upon release from harmonic traps. In swave systems, where theorder parameter is a complex scalar, we find that the interference patternsdepend on the relative phase of the order parameters of the condensates. Inp-wave systems involving the mixture of two-hyperfine states, we show that theinterference pattern exhibits a polarization effect depending on the relativeorientation of the two vector order parameters. Lastly, we also point out thatp-wave Fermi condensates exhibit an anisotropic expansion, reflecting thespatial anisotropy of the underlying interaction between fermions and theorbital nature of the vector order parameter. Potential applications of ourresults include systems of ultra-cold atoms that exhibit p-wave Feshbachresonances such as 6Li or 40K.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Spatially extended Ly-alpha sources that are faint and/or compact in coninuumare candidates for extremely young (~< 10^7 yrs) galaxies at high redshifts. Wepresent medium-resolution (R~2000) spectroscopy of such extended Ly-alphasources found in our previous study at z~3-5, using VLT/VIMOS. The deepspectroscopy showed that all 18 objects we observed have large equivalentwidths (EWs) exceeding 100 A. For about 30% of our sample (five objects), weidentified conspicuous asymmetry on the profiles of the Ly-alpha line. Theyshow broad wing emission components on the red side, and sharp cut-off on theblue side of the Ly-alpha line. Such asymmetry is often seen in superwindgalaxies known to date, and also consistent with a theoretical prediction ofsuperwind activity. There are eight objects (8/18 ~ 40%) that have large EWsexceeding 200 A, and no clear signature of superwind activities. Such large EWscannot be explained in terms of photo-ionization by a moderately old (>10^7yrs) stellar population, even with a top-heavy IMF or an extremely lowmetallicity. These eight objects clearly show a positive correlation betweenthe Ly-alpha luminosity and the velocity width. This suggests that these eightobjects are good candidates for forming-galaxies in a gas-cooling phase.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We study the evolution and saturation of the gluon distribution function inthe quark-gluon plasma as probed by a propagating parton and its effect on thecomputation of jet quenching or transport parameter $\\hat{q}$. For thermalpartons, the saturation scale $Q^2_s$ is found to be proportional to the Debyescreening mass $\\mu_D^2$. For hard probes, evolution at small $x=Q^2_s/6ET$leads to jet energy dependence of $\\hat{q}$. We study this dependence for botha conformal gauge theory in weak and strong coupling limit and for (pure gluon)QCD. The energy dependence can be used to extract the shear viscosity $\\eta$ ofthe medium since $\\eta$ can be related to the transport parameter for thermalpartons in a transport description. We also derive upper bounds on thetransport parameter for both energetic and thermal partons. The later leads toa lower bound on shear viscosity-to-entropy density ratio which is consistentwith the conjectured lower bound $\\eta/s\\geq 1/4\\pi$. We also discuss theimplications on the study of jet quenching at the BNL Relativistic Heavy IonCollider and the CERN Large Hadron Collider and the bulk properties of thedense matter.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Modifications to quark and antiquark fragmentation functions due toquark-quark (antiquark) double scattering in nuclear medium are studiedsystematically up to order \\cal{O}(\\alpha_{s}^2)$ in deeply inelasticscattering (DIS) off nuclear targets. At the order $\\cal{O}(\\alpha_s^2)$,twist-four contributions from quark-quark (antiquark) rescattering also exhibitthe Landau-Pomeranchuck-Midgal (LPM) interference feature similar to gluonbremsstrahlung induced by multiple parton scattering. Compared to quark-gluonscattering, the modification, which is dominated by $t$-channel quark-quark(antiquark) scattering, is only smaller by a factor of $C_F/C_A=4/9$ times theratio of quark and gluon distributions in the medium. Such a modification isnot negligible for realistic kinematics and finite medium size. Themodifications to quark (antiquark) fragmentation functions from quark-antiquarkannihilation processes are shown to be determined by the antiquark (quark)distribution density in the medium. The asymmetry in quark and antiquarkdistributions in nuclei will lead to different modifications of quark andantiquark fragmentation functions inside a nucleus, which qualitativelyexplains the experimentally observed flavor dependence of the leading hadronsuppression in semi-inclusive DIS off nuclear targets. The quark-antiquarkannihilation processes also mix quark and gluon fragmentation functions in thelarge fractional momentum region, leading to a flavor dependence of jetquenching in heavy-ion collisions.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Of the nearby transiting exoplanets that are amenable to detailed study,TrES-2 is both the most massive and has the largest impact parameter. Wepresent z-band photometry of three transits of TrES-2. We improve upon theestimates of the planetary, stellar, and orbital parameters, in conjunctionwith the spectroscopic analysis of the host star by Sozzetti and co-workers. Wefind the planetary radius to be 1.222 +/- 0.038 R_Jup and the stellar radius tobe 1.003 +/- 0.027 R_Sun. The quoted uncertainties include the systematic errordue to the uncertainty in the stellar mass (0.980 +/- 0.062 M_Sun). The timingsof the transits have an accuracy of 25s and are consistent with a uniformperiod, thus providing a baseline for future observations with the NASA Keplersatellite, whose field of view will include TrES-2.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "In this work, we introduce a special kind of quantum cloning machine calledHybrid quantum cloning machine. The introduced Hybrid quantum cloning machineor transformation is nothing but a combination of pre-existing quantum cloningtransformations. In this sense it creates its own identity in the field ofquantum cloners. Hybrid quantum cloning machine can be of two types: (i) Statedependent and (ii) State independent or Universal. We study here the above twotypes of Hybrid quantum cloning machines. Later we will show that the statedependent hybrid quantum-cloning machine can be applied on only four inputstates. We will also find in this paper another asymmetric universal quantumcloning machine constructed from the combination of optimal universal B-Hquantum cloning machine and universal anti-cloning machine. The fidelities ofthe two outputs are different and their values lie in the neighborhood of${5/6} $", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "\"Extended Clifford algebras\" are introduced as a means to obtain low MLdecoding complexity space-time block codes. Using left regular matrixrepresentations of two specific classes of extended Clifford algebras, twosystematic algebraic constructions of full diversity Distributed Space-TimeCodes (DSTCs) are provided for any power of two number of relays. The leftregular matrix representation has been shown to naturally result in space-timecodes meeting the additional constraints required for DSTCs. The DSTCs soconstructed have the salient feature of reduced Maximum Likelihood (ML)decoding complexity. In particular, the ML decoding of these codes can beperformed by applying the lattice decoder algorithm on a lattice of four timeslesser dimension than what is required in general. Moreover these codes have auniform distribution of power among the relays and in time, thus leading to alow Peak to Average Power Ratio at the relays.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "In the coming decades, research in extrasolar planets aims to advance twogoals: 1) detecting and characterizing low-mass planets increasingly similar tothe Earth, and 2) improving our understanding of planet formation. We present anew planet detection method that is capable of making large advances towardsboth of these objectives and describe a modest network of telescopes that isable to make the requisite observations. In a system where a known planettransits its host star, a second planet in that system will cause the timebetween transits to vary. These transit timing variations can be used to inferthe orbital elements and mass of the perturbing planet even if it has a massthat is smaller than the mass of the Earth. This detection techniquecomplements other techniques because it is most sensitive in mean-motionresonances where, due to degeneracies, other techniques have reducedsensitivity. Small ground-based observatories have already exceeded thephotometric precision necessary to detect sub-Earth mass planets. However, TTVplanet searches are currently limited by the relatively small number ofhigh-precision transit data and insufficient observing time on existingtelescopes. These issues will be compounded as the number of known transitingplanets suitable for TTV study will increase substantially in the near future.A relatively modest investment in a ground-based network of small ($\\sim 0.5{\\rm m}$ telescopes could provide the needed coverage and so dramaticallyincrease the effectiveness of transit timing observations.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Intermediate resolution spectroscopy of the white dwarfSDSSJ104341.53+085558.2 contains double-peaked emission lines ofCaII8498,8542,8662 and identifies this object to be the second single whitedwarf to be surrounded by a gaseous disc of metal-rich material, similar to therecently discovered SDSSJ1228+1040. A photospheric Magnesium abundance of 0.3times the solar value, determined from the observed MgII4481 absorption line,implies that the white dwarf is accreting from the circumstellar material. Theabsence of Balmer emission lines and of photospheric HeI4471 absorptionindicates that the accreted material is depleted in volatile elements and, byanalogy with SDSS1228+1040, may be the result of the tidal disruption of anasteroid. Additional spectroscopy of the DAZ white dwarfs WD1337+705 and GD362does not reveal CaII emission lines. GD362 is one of the few cool DAZ thatdisplay strong infrared flux excess, thought to be originating in acircumstellar dust disc, and its temperature is likely too low to sublimatesufficient amounts of disc material to generate detectable CaII emission.WD1337+705 is, as SDSS1228+1040 and SDSS1043+0855, moderately hot, but has thelowest Mg abundance of those three stars, suggesting a possible correlationbetween the photospheric Mg abundance and the equivalent width of the CaIIemission triplet. Our inspection of 7360 white dwarfs from SDSS DR4 fails tounveil additional strong \"metal gas disc\" candidates, and implies that theseobjects are rather rare.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The PTCDA (3,4,9,10-Perylene-tetracarboxylic dianhydride) and the NTCDA(1,4,5,8-Naphtalenetetracarboxylic dianhydride) are aromatic, stable, planarand highly symmetric with unusual electrical properties. The PTCDA is asemiconductor organic crystalline of particular interest due to its excellentproperties and electronic potential that are used in optoelectronic devices andthe NTCDA it is monoclinic and its space group is similar to that of the PTCDA.Recently, alternate layers of PTCDA and NTCDA were growth forming multiplestructures of quantum wells showing a new class of materials with new opticlineal properties. Some have assured that their big utilities would be centeredin the construction of diodes and of possible guides of waves. We have carriedout calculations semi-empirical of the electronic structures and of opticproperties of the PTCDA and of the NTCDA that show us that they are structureshighly orderly polymeric, semiconductors in a negative load state (chargestate= -2)", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The distribution of galaxies in position and velocity around the centers ofgalaxy clusters encodes important information about cluster mass and structure.Using the maxBCG galaxy cluster catalog identified from imaging data obtainedin the Sloan Digital Sky Survey, we study the BCG-galaxy velocity correlationfunction. By modeling its non-Gaussianity, we measure the mean and scatter invelocity dispersion at fixed richness. The mean velocity dispersion increasesfrom 202+/-10 km/s for small groups to more than 854+/-102 km/s for largeclusters. We show the scatter to be at most 40.5+/-3.5%, declining to14.9+/-9.4% in the richest bins. We test our methods in the C4 cluster catalog,a spectroscopic cluster catalog produced from the Sloan Digital Sky Survey DR2spectroscopic sample, and in mock galaxy catalogs constructed from N-bodysimulations. Our methods are robust, measuring the scatter to well withinone-sigma of the true value, and the mean to within 10%, in the mock catalogs.By convolving the scatter in velocity dispersion at fixed richness with theobserved richness space density function, we measure the velocity dispersionfunction of the maxBCG galaxy clusters. Although velocity dispersion andrichness do not form a true mass-observable relation, the relationship betweenvelocity dispersion and mass is theoretically well characterized and has lowscatter. Thus our results provide a key link between theory and observations upto the velocity bias between dark matter and galaxies.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "A complex manifold Y satisfies the Convex Approximation Property (CAP) ifevery holomorphic map from a neighborhood of a compact convex set K in acomplex Euclidean space C^n to Y can be approximated, uniformly on K, by entiremaps from C^n to Y. If X is a reduced Stein space and Z is a stratifiedholomorphic fiber bundle over X all of whose fibers satisfy CAP, then sectionsof Z over X enjoy the Oka property with (jet) interpolation and approximation.Previously this has been proved by the author in the case when X is a Steinmanifold without singularities (Ann. Math., 163 (2006), 689-707,math.CV/0402278; Ann. Inst. Fourier, 55 (2005), 733-751, math.CV/0411048). Wealso give existence results for holomorphic sections under certain connectivityhypothesis on the fibers. In the final part of the paper we obtain the Okaproperty for sections of submersions with stratified sprays over Stein spaces.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "When a family of non symmetrical heterocycled compounds is investigated, avariety of mesophases can be observed with rather different features. Here wereport the behaviour of seven different members among a family of suchmaterials, that consists of mesomorphic oxadiazole compounds. In two of thesecompounds, the optical microscope investigation shows very interestingbehaviours. In their smectic phases, fan-shaped and toric textures, sometimeswith periodic instability, are observed. Moreover, the nematic phase displays atexture transition. Texture transitions have been previously observed onlyinside the nematic phase of some compounds belonging to the families of theoxybenzoic and cyclohexane acids. In these two oxadiazole compounds we canobserve what we define as a \"toric nematic phase\", heating the samples from thesmectic phase. The toric nematic texture disappears as the sample is furtherheated, changing into a smooth texture.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We study the effect of continuous quantum error correction in the case whereeach qubit in a codeword is subject to a general Hamiltonian interaction withan independent bath. We first consider the scheme in the case of a trivialsingle-qubit code, which provides useful insights into the workings ofcontinuous error correction and the difference between Markovian andnon-Markovian decoherence. We then study the model of a bit-flip code with eachqubit coupled to an independent bath qubit and subject to continuouscorrection, and find its solution. We show that for sufficiently largeerror-correction rates, the encoded state approximately follows an evolution ofthe type of a single decohering qubit, but with an effectively decreasedcoupling constant. The factor by which the coupling constant is decreasedscales quadratically with the error-correction rate. This is compared to thecase of Markovian noise, where the decoherence rate is effectively decreased bya factor which scales only linearly with the rate of error correction. Thequadratic enhancement depends on the existence of a Zeno regime in theHamiltonian evolution which is absent in purely Markovian dynamics. We analyzethe range of validity of this result and identify two relevant time scales.Finally, we extend the result to more general codes and argue that theperformance of continuous error correction will exhibit the same qualitativecharacteristics.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We report a high-resolution neutron diffraction study on theorbitally-degenerate spin-1/2 hexagonal antiferromagnet AgNiO2. A structuraltransition to a tripled unit cell with expanded and contracted NiO6 octahedraindicates root(3) x root(3) charge order on the Ni triangular lattice. Thissuggests charge order as a possible mechanism of lifting the orbital degeneracyin the presence of charge fluctuations, as an alternative to Jahn-Tellerdistortions. A novel magnetic ground state is observed at base temperatureswith the electron-rich S = 1 Ni sites arranged in alternating ferromagneticrows on a triangular lattice, surrounded by a honeycomb network of non-magneticand metallic Ni ions. We also report first-principles band-structurecalculations that explain microscopically the origin of these phenomena.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We propose that Crab giant pulses are generated on closed magnetic fieldlines near the light cylinder via anomalous cyclotron resonance on the ordinarymode. Waves are generated in a set of fine, unequally spaced, narrow emissionbands at frequencies much lower than a local cyclotron frequency. Location ofemission bands is fitted to spectral structures seen by Eilek et al. (2006).  To reproduce the data, the required density of plasma in the giant pulsesemission region is much higher, by a factor $\\sim 3 \\times 10^5$, than theminimal Goldreich-Julian density. Emission is generated by a population ofhighly energetic particles with radiation-limited Lorentz factors $\\gamma \\sim7 \\times 10^7$, produced during occasional reconnection close to the Y point,where the last closed field lines approach the light cylinder.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "It has been shown that the luminosity of AGNs and the size of their broadline region obey a simple relation of the type R=a L^g, from faint Seyfertnuclei to bright quasars, allowing single-epoch determination of the centralblack hole mass M=b L^g D^2 from their luminosity L and width of H_betaemission line. Adopting this mass determination for cosmological studiesrequires the extrapolation to high z and L of a relation whose calibrationrelies so far on reverberation mapping measurements performed for L<10^46 erg/sand z<0.4. We initiated a campaign for the monitoring of a few luminous,intermediate z quasars whose apparent magnitude V<15.7 allows observations witha 1.8m telescope, aimed at proving that emission lines vary and respond tocontinuum variations even for luminosities >10^47 erg/s, and determiningeventually their M_BH from reverberation mapping. We have repeatedly performedsimultaneous observations of quasars and reference stars to determine relativevariability of continuum and emission lines. We describe the observations andmethods of analysis. For the quasars PG1634+706 and PG1247+268 we obtainlight-curves respectively for CIII], MgII and for CIV, CIII] emission lineswith the relevant continua. During 3.2 years of observation, in the former caseno continuum variability has been detected and the evidence for linevariability is marginal, while in the latter case both continuum and linevariability are detected with high significance and the line variations appearcorrelated with continuum variations. The detection of the emission linevariability in a quasar with L~10^47 erg/s encourages the prosecution of thecampaign which should provide a black hole mass estimate in other 5-6 years,constraining the M_BH-L relation in a poorly explored range of luminosity.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We microscopically model the decoherence dynamics of entangled coherentstates under the influence of vacuum fluctuation. We derive an exact masterequation with time-dependent coefficients reflecting the memory effect of theenvironment, by using the Feynman-Vernon influence functional theory in thecoherent-state representation. Under the Markovian approximation, our masterequation recovers the widely used Lindblad equation in quantum optics. We theninvestigate the non-Markovian entanglement dynamics of the quantum channel interms of the entangled coherent states under noise. Compared with the resultsin Markovian limit, it shows that the non-Markovian effect enhances thedisentanglement to the initially entangled coherent state. Our analysis alsoshows that the decoherence behaviors of the entangled coherent states dependsensitively on the symmetrical properties of the entangled coherent states aswell as the interactions between the system and the environment.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Cell colonies of bacteria, tumour cells and fungi, under nutrient limitedgrowth conditions, exhibit complex branched growth patterns. In order toinvestigate this phenomenon we present a simple hybrid cellular automaton modelof cell colony growth. In the model the growth of the colony is limited by anutrient that is consumed by the cells and which inhibits cell division if itfalls below a certain threshold. Using this model we have investigated how thenutrient consumption rate of the cells affects the growth dynamics of thecolony. We found that for low consumption rates the colony takes on a Eden-likemorphology, while for higher consumption rates the morphology of the colony isbranched with a fractal geometry. These findings are in agreement with previousresults, but the simplicity of the model presented here allows for a linearstability analysis of the system. By observing that the local growth of thecolony is proportional to the flux of the nutrient we derive an approximatedispersion relation for the growth of the colony interface. This dispersionrelation shows that the stability of the growth depends on how far the nutrientpenetrates into the colony. For low nutrient consumption rates the penetrationdistance is large, which stabilises the growth, while for high consumptionrates the penetration distance is small, which leads to unstable branchedgrowth. When the penetration distance vanishes the dispersion relation isreduced to the one describing Laplacian growth without ultra-violetregularisation. The dispersion relation was verified by measuring how theaverage branch width depends on the consumption rate of the cells and showsgood agreement between theory and simulations.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We study the cosmological evolution of a tachyon scalar field T with aDirac-Born-Infeld type lagrangian and potential V(T) coupled to a canonicallynormalized scalar field \\phi with an arbitrary interaction term B(T,\\phi) inthe presence of a barotropic fluid $\\rb$, which can be matter or radiation. Theforce between the barotropic fluid and the scalar fields is only gravitational.We show that the dynamics is completely determine by only three parameters L1 =- V_T/ V^{3/2}, L2= - B_T /B^{3/2} and L3 =-B_{\\phi}/B. We determineanalytically theconditions for $\\lm_i$ under which the energy density of T,\\phi and $\\rb$ have the same redshift. We study the behavior of T and \\phi inthe asymptotic limits for L_i and we show the numerical solution for differentinteresting cases.  The effective equation of state for the tachyon field changes due to theinteraction with the scalar field and we show that it is possible for a tachyonfield to redshift as matter in the absence of an interaction term B and asradiation when B is turned on. This result solves then the tachyonic matterproblem.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "In this paper, a game-theoretic model for studying power control for wirelessdata networks in frequency-selective multipath environments is analyzed. Theuplink of an impulse-radio ultrawideband system is considered. The effects ofself-interference and multiple-access interference on the performance of Rakereceivers are investigated for synchronous systems. Focusing on energyefficiency, a noncooperative game is proposed in which users in the network areallowed to choose their transmit powers to maximize their own utilities, andthe Nash equilibrium for the proposed game is derived. It is shown that, due tothe frequency selective multipath, the noncooperative solution is achieved atdifferent signal-to-interference-plus-noise ratios, respectively of the channelrealization. A large-system analysis is performed to derive explicitexpressions for the achieved utilities. The Pareto-optimal (cooperative)solution is also discussed and compared with the noncooperative approach.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We study the relaxational critical dynamics of the three-dimensional randomanisotropy magnets with the non-conserved n-component order parameter coupledto a conserved scalar density. In the random anisotropy magnets the structuraldisorder is present in a form of local quenched anisotropy axes of randomorientation. When the anisotropy axes are randomly distributed along the edgesof the n-dimensional hypercube, asymptotical dynamical critical propertiescoincide with those of the random-site Ising model. However structural disordergives rise to considerable effects for non-asymptotic critical dynamics. Weinvestigate this phenomenon by a field-theoretical renormalization groupanalysis in the two-loop order. We study critical slowing down and obtainquantitative estimates for the effective and asymptotic critical exponents ofthe order parameter and scalar density. The results predict complex scenariosfor the effective critical exponent approaching an asymptotic regime.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present spectroscopic observations of a massive globular cluster in thedwarf irregular galaxy Sextans B, discovered by us on Hubble Space TelescopeWide Field and Planetary Camera 2 (HST WFPC2) images. Long-slit spectra wereobtained with the SCORPIO spectrograph on the the 6-m telescope at the SpecialAstrophysical observatory of the Russian Academy of Sciences. We determine age,metallicity and alpha-element abundance ratio for the globular cluster to be $2 \\pm 1$ Gyr, $-1.35 \\pm 0.25$ dex, and $ 0.1 \\pm 0.1$ dex, respectively. Mainphotometric and structural parameters of it were determined using our surfacephotometry on the HST images. The mass ($\\sim 10^5 M \\sun$), luminosity andstructural parameters appear to be typical for the globular clusters in our ownGalaxy. Our findings shed a new light on the evolutionary history of Sextans B.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Spatially resolved studies of star forming regions show that the assumptionof spherical geometry is not realistic in most cases, with a major complicationposed by the gas being ionised by multiple non-centrally located stars or starclusters. We try to isolate the effects of multiple non-centrally located starson the temperature and ionisation structure of HII regions, via theconstruction of 3D photoionisation models using the 3D Monte Carlophotoionisation code MOCASSIN. We find that the true temperature fluctuationsdue to the stellar distribution (as opposed to the large-scale temperaturegradients due to other gas properties) are small in all cases and not asignificant cause of error in metallicity studies. Strong emission lines fromHII regions are often used to study the metallicity of star-forming regions. Wecompare integrated emission line spectra from our models and quantify anysystematic errors caused by the simplifying assumption of a single, centrallocation for all ionising sources. We find that the dependence of themetallicity indicators on the ionisation parameter causes a clear bias, due tothe fact that models with a fully distributed configuration of stars alwaysdisplay lower ionisation parameters than their fully concentrated counterparts.The errors found imply that the geometrical distribution of ionisation sourcesmay partly account for the large scatter in metallicities derived usingmodel-calibrated empirical methods.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The purpose of this paper is to assess the statistical characterization ofweighted networks in terms of the generalization of the relevant parameters,namely average path length, degree distribution and clustering coefficient.Although the degree distribution and the average path length admitstraightforward generalizations, for the clustering coefficient severaldifferent definitions have been proposed in the literature. We examined thedifferent definitions and identified the similarities and differences betweenthem. In order to elucidate the significance of different definitions of theweighted clustering coefficient, we studied their dependence on the weights ofthe connections. For this purpose, we introduce the relative perturbation normof the weights as an index to assess the weight distribution. This studyrevealed new interesting statistical regularities in terms of the relativeperturbation norm useful for the statistical characterization of weightedgraphs.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Information integration applications, such as mediators or mashups, thatrequire access to information resources currently rely on users manuallydiscovering and integrating them in the application. Manual resource discoveryis a slow process, requiring the user to sift through results obtained viakeyword-based search. Although search methods have advanced to include evidencefrom document contents, its metadata and the contents and link structure of thereferring pages, they still do not adequately cover information sources --often called ``the hidden Web''-- that dynamically generate documents inresponse to a query. The recently popular social bookmarking sites, which allowusers to annotate and share metadata about various information sources, providerich evidence for resource discovery. In this paper, we describe aprobabilistic model of the user annotation process in a social bookmarkingsystem del.icio.us. We then use the model to automatically find resourcesrelevant to a particular information domain. Our experimental results on dataobtained from \\emph{del.icio.us} show this approach as a promising method forhelping automate the resource discovery task.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We obtain constraints on possible structures of mass matrices in the quarksector by using as experimental restrictions the determined values of the quarkmasses at the $M_Z$ energy scale, the magnitudes of the quark mixing matrixelements $V_{\\rm ud}$, $V_{\\rm us}$, $V_{\\rm cd}$, and $V_{\\rm cs}$, and theJarlskog invariant $J(V)$. Different cases of specific mass matrices areexamined in detail. The quality of the fits for the Fritzsch and Stech typemass matrices is about the same with $\\chi^2/{\\rm dof}=4.23/3=1.41$ and$\\chi^2/{\\rm dof}=9.10/4=2.28$, respectively. The fit for a simplegeneralization (one extra parameter) of the Fritzsch type matrices, in thephysical basis, is much better with $\\chi^2/{\\rm dof}=1.89/4=0.47$. Forcomparison we also include the results using the quark masses at the 2 GeVenergy scale. The fits obtained at this energy scale are similar to that at$M_Z$ energy scale, implying that our results are unaffected by the evolutionof the quark masses from 2 to 91 GeV.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "A generalization of the usual ideles group is proposed, namely, we constructcertain adelic complexes for sheaves of $K$-groups on schemes. More generally,such complexes are defined for any abelian sheaf on a scheme. We focus on thecase when the sheaf is associated to the presheaf of a homology theory withcertain natural axioms, satisfied by $K$-theory. In this case it is proven thatthe adelic complex provides a flasque resolution for the above sheaf and thatthe natural morphism to the Gersten complex is a quasiisomorphism. The mainadvantage of the new adelic resolution is that it is contravariant andmultiplicative in contrast to the Gersten resolution. In particular, thisallows to reprove that the intersection in Chow groups coincides up to signwith the natural product in the corresponding $K$-cohomology groups. Also, weshow that the Weil pairing can be expressed as a Massey triple product in$K$-cohomology groups with certain indices.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We here report on the multiwavelength study which led us to theidentification of X-ray source IGR J16194-2810 as a new Symbiotic X-ray Binary(SyXB), that is, a rare type of Low Mass X-ray Binary (LMXB) composed of aM-type giant and a compact object. Using the accurate X-ray position allowed bySwift/XRT data, we pinpointed the optical counterpart, a M2 III star. Besides,the combined use of the spectral information afforded by XRT and INTEGRAL/IBISshows that the 0.5-200 keV spectrum of this source can be described with anabsorbed Comptonization model, usually found in LMXBs and, in particular, inSyXBs. No long-term (days to months) periodicities are detected in the IBISdata. The time coverage afforded by XRT reveals shot-noise variability typicalof accreting Galactic X-ray sources, but is not good enough to explore thepresence of X-ray short-term (seconds to hours) oscillations in detail. Byusing the above information, we infer important parameters for this source suchas its distance (about 3.7 kpc) and X-ray luminosity (about 1.4e35 erg/s in the0.5-200 keV band), and we give a description for this system (typical of SyXBs)in which a compact object (possibly a neutron star) accretes from the wind ofits M-type giant companion. We also draw some comparisons between IGRJ16194-2810 and other sources belonging to this subclass, finding that thisobject resembles SyXBs 4U 1700+24 and 4U 1954+31.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Since the advent of chirped pulse amplification1 the peak power of lasers hasgrown dramatically and opened the new branch of high field science, deliveringthe focused irradiance, electric fields of which drive electrons into therelativistic regime. In a plasma wake wave generated by such a laser,modulations of the electron density naturally and robustly take the shape ofparaboloidal dense shells, separated by evacuated regions, moving almost at thespeed of light. When we inject another counter-propagating laser pulse, it ispartially reflected from the shells, acting as relativistic flying(semi-transparent) mirrors, producing an extremely time-compressedfrequency-multiplied pulse which may be focused tightly to the diffractionlimit. This is as if the counterstreaming laser pulse bounces off arelativistically swung tennis racket, turning the ball of the laser photonsinto another ball of coherent X-ray photons but with a form extremelyrelativistically compressed to attosecond and zeptosecond levels. Here wereport the first demonstration of the frequency multiplication detected fromthe reflection of a weak laser pulse in the region of the wake wave generatedby the driver pulse in helium plasma. This leads to the possibility of verystrong pulse compression and extreme coherent light intensification. ThisRelativistic Tennis with photon beams is demonstrated leading to thepossibility toward reaching enormous electromagnetic field intensification andfinally approaching the Schwinger field, toward which the vacuum nonlinearlywarps and eventually breaks, producing electron-positron pairs.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The noteworthy BaBar and Belle evidence for $D^0$-$\\bar{D}^0$ mixingmotivates us to study its impact on $D^0\\to K^{*\\pm} K^\\mp$ decays and theirCP-conjugate processes. We show that both the $D^0$-$\\bar{D}^0$ mixingparameters ($x$ and $y$) and the strong phase difference between $\\bar{D}^0\\toK^{*\\pm}K^\\mp$ and $D^0\\to K^{*\\pm}K^\\mp$ transitions ($\\delta$) can bedetermined or constrained from the time-dependent measurements of these decaymodes. On the $\\psi (3770)$ and $\\psi (4140)$ resonances at a $\\tau$-charmfactory, it is even possible to determine or constrain $x$, $y$ and $\\delta$from the time-independent measurements of coherent $(D^0\\bar{D}^0) \\to(K^{*\\pm} K^\\mp)(K^{*\\pm} K^\\mp)$ decays. If the CP-violating phase of$D^0$-$\\bar{D}^0$ mixing is significant in a scenario beyond the standardmodel, it can also be extracted from the $K^{*\\pm} K^\\mp$ events.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Dynamic properties of molecular motors that fuel their motion by activelyinteracting with underlying molecular tracks are studied theoretically viadiscrete-state stochastic ``burnt-bridge'' models. The transport of theparticles is viewed as an effective diffusion along one-dimensional latticeswith periodically distributed weak links. When an unbiased random walker passesthe weak link it can be destroyed (``burned'') with probability p, providing abias in the motion of the molecular motor. A new theoretical approach thatallows one to calculate exactly all dynamic properties of motor proteins, suchas velocity and dispersion, at general conditions is presented. It is foundthat dispersion is a decreasing function of the concentration of bridges, whilethe dependence of dispersion on the burning probability is more complex. Ourcalculations also show a gap in dispersion for very low concentrations of weaklinks which indicates a dynamic phase transition between unbiased and biaseddiffusion regimes. Theoretical findings are supported by Monte Carlo computersimulations.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "On a fading channel with no channel state information at the receiver,calculating true log-likelihood ratios (LLR) is complicated. Existing workassume that the power of the additive noise is known and use the expected valueof the fading gain in a linear function of the channel output to findapproximate LLRs. In this work, we first assume that the power of the additivenoise is known and we find the optimum linear approximation of LLRs in thesense of maximum achievable transmission rate on the channel. The maximumachievable rate under this linear LLR calculation is almost equal to themaximum achievable rate under true LLR calculation. We also observe that thismethod appears to be the optimum in the sense of bit error rate performancetoo. These results are then extended to the case that the noise power isunknown at the receiver and a performance almost identical to the case that thenoise power is perfectly known is obtained.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Many important real-world networks manifest \"small-world\" properties such asscale-free degree distributions, small diameters, and clustering. The mostcommon model of growth for these networks is \"preferential attachment\", wherenodes acquire new links with probability proportional to the number of linksthey already have. We show that preferential attachment is a special case ofthe process of molecular evolution. We present a new single-parameter model ofnetwork growth that unifies varieties of preferential attachment with thequasispecies equation (which models molecular evolution), and also with theErdos-Renyi random graph model. We suggest some properties of evolutionarymodels that might be applied to the study of networks. We also derive the formof the degree distribution resulting from our algorithm, and we show throughsimulations that the process also models aspects of network growth. Theunification allows mathematical machinery developed for evolutionary dynamicsto be applied in the study of network dynamics, and vice versa.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The problem of finding the asymptotic behavior of the maximal density ofsphere packings in high Euclidean dimensions is one of the most fascinating andchallenging problems in discrete geometry. One century ago, Minkowski obtaineda rigorous lower bound that is controlled asymptotically by $1/2^d$, where $d$is the Euclidean space dimension. An indication of the difficulty of theproblem can be garnered from the fact that exponential improvement ofMinkowski's bound has proved to be elusive, even though existing upper boundssuggest that such improvement should be possible. Using astatistical-mechanical procedure to optimize the density associated with a\"test\" pair correlation function and a conjecture concerning the existence ofdisordered sphere packings [S. Torquato and F. H. Stillinger, ExperimentalMath. {\\bf 15}, 307 (2006)], the putative exponential improvement was foundwith an asymptotic behavior controlled by $1/2^{(0.77865...)d}$. Using the samemethods, we investigate whether this exponential improvement can be furtherimproved by exploring other test pair correlation functions correponding todisordered packings. We demonstrate that there are simpler test functions thatlead to the same asymptotic result. More importantly, we show that there is awide class of test functions that lead to precisely the same exponentialimprovement and therefore the asymptotic form $1/2^{(0.77865...)d}$ is muchmore general than previously surmised.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We study macroscopic quantum tunneling (MQT) in c-axis twist Josephsonjunctions made of high-T_c superconductors in order to clarify the influence ofthe anisotropic order parameter symmetry (OPS) on MQT. The dependence of theMQT rate on the twist angle $\\gamma$ about the c-axis is calculated by usingthe functional integral and the bounce method. Due to the d-wave OPS, the$\\gamma$ dependence of standard deviation of the switching current distributionand the crossover temperature from thermal activation to MQT are found to begiven by $\\cos2\\gamma$ and $\\sqrt{\\cos2\\gamma}$, respectively. We also showthat a dissipative effect resulting from the nodal quasiparticle excitation onMQT is negligibly small, which is consistent with recent MQT experiments usingBi${}_2$Sr${}_2$CaCu${}_2$O${}_{8 + \\delta}$ intrinsic junctions. These resultsindicate that MQT in c-axis twist junctions becomes a useful experimental toolfor testing the OPS of high-T_c materials at low temperature, and suggest highpotential of such junctions for qubit applications.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "In the semi-classical treatment, i.e. in a classical black hole geometry,Hawking quanta emerge from trans-Planckian configurations because of scaleinvariance. There is indeed no scale to stop the blue-shifting effectencountered in the backward propagation towards the event horizon. On thecontrary, when taking into account the gravitational interactions neglected inthe semi-classical treatment, a UV scale stopping the blue-shift could bedynamically engendered. To show that this is the case, we use anon-perturbative treatment based on the large-N limit, where $N$ is the numberof matter fields. In this limit, the semi-classical treatment is the leadingcontribution. Non-linear gravitational effects appear in the next orders and inthe first of these, the effects are governed by the two-point correlationfunction of the energy-momentum tensor evaluated in the vacuum. Taking thiscorrelator into account, backward propagated modes are dissipated at a distancefrom the horizon $\\propto G\\kappa$ when measured in a freely falling frame.($G$ is Newton's constant and $\\kappa$ the surface gravity.) This result can bealso obtained by considering light propagation in a stochastic ensemble ofmetrics whose fluctuations are determined by the above correlator.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We propose an extension of the principle of virtual work of mechanics torandom dynamics of mechanical systems. The total virtual work of theinteracting forces and inertial forces on every particle of the system iscalculated by considering the motion of each particle. Then according to theprinciple of Lagrange-d'Alembert for dynamical equilibrium, the vanishingensemble average of the virtual work gives rise to the thermodynamicequilibrium state with maximization of thermodynamic entropy. This approachestablishes a close relationship between the maximum entropy approach forstatistical mechanics and a fundamental principle of mechanics, and constitutesan attempt to give the maximum entropy approach, considered by many as only aninference principle based on the subjectivity of probability and entropy, thestatus of fundamental physics law.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "With an automatic image analysis device, we studied the temporal distributionof the locomotor activity of E. orientalis and E. vuilleti during 24 h, andover several days to know whether the activity rhythms of these two Eupelmidaeplay a role in their competitive interactions. The analysis of locomotoractivity rhythms of E. orientalis and E. vuilleti shows that the locomotoractivity of both species presents daily cyclic variations. These two Eupelmidaehave similar activity rhythms. Displacements of these parasitoids essentiallytake place during the photophase. But the activity of E. vuilleti is earlier,because the individuals of this species start their activity on average 4 to 5h earlier than those of E. orientalis. E. vuilleti begins its displacementsseveral hours before the onset of lighting, whereas E. orientalis is activeonly in the presence of the light. This shift of starting activity is thus afactor allowing these concurrent species to minimize their interactions duringthe cohabitation period in traditional granaries after the harvests of cowpea.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "It has been demonstrated that quantum vacuum energy gravitates according tothe equivalence principle, at least for the finite Casimir energies associatedwith perfectly conducting parallel plates. We here add further support to thisconclusion by considering parallel semitransparent plates, that is,delta-function potentials, acting on a massless scalar field, in a spacetimedefined by Rindler coordinates (tau,x,y,xi). Fixed xi in such a spacetimerepresents uniform acceleration. We calculate the force on systems consistingof one or two such plates at fixed values of xi. In the limit of large Rindlercoordinate xi (small acceleration), we recover (via the equivalence principle)the situation of weak gravity, and find that the gravitational force on thesystem is just Mg, where g is the gravitational acceleration and M is the totalmass of the system, consisting of the mass of the plates renormalized by theCasimir energy of each plate separately, plus the energy of the Casimirinteraction between the plates. This reproduces the previous result in thelimit as the coupling to the delta-function potential approaches infinity.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "This paper extends earlier work on quantum theory representations of naturalnumbers N, integers I, and rational numbers Ra to describe a space of theserepresentations and transformations on the space. The space is parameterized by4-tuple points in a parameter set. Each point, (k,m,h,g), labels a specificrepresentation of X = N, I, Ra as a Fock space F^{X}_{k,m,h} of states offinite length strings of qukits q and a string state basis B^{X}_{k,m,h,g}. Thepair (m,h) locates the q string in a square integer lattice I \\times I, k isthe q base, and the function g fixes the gauge or basis states for each q. Mapson the parameter set induce transformations on on the representation space.There are two shifts, a base change operator W_{k',k}, and a basis or gaugetransformation function U_{k}. The invariance of the axioms and theorems for N,I, and Ra under any transformation is discussed along with the dependence ofthe properties of W_{k',k} on the prime factors of k' and k. This suggests thatone consider prime number q's, q_{2}, q_{3}, q_{5}, etc. as elementary and thebase k q's as composites of the prime number q's.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We use a N--body/hydrodynamic simulation to forecast the future encounterbetween the Milky Way and the Andromeda galaxies, given current observationalconstraints on their relative distance, relative velocity, and masses. Allowingfor a comparable amount of diffuse mass to fill the volume of the Local Group,we find that the two galaxies are likely to collide in a few billion years -within the Sun's lifetime. During the the interaction, there is a chance thatthe Sun will be pulled away from its present orbital radius and reside in anextended tidal tail. The likelihood for this outcome increases as the mergerprogresses, and there is a remote possibility that our Sun will be more tightlybound to Andromeda than to the Milky Way before the final merger. Eventually,after the merger has completed, the Sun is most likely to be scattered to theouter halo and reside at much larger radii (>30 kpc). The density profiles ofthe stars, gas and dark matter in the merger product resemble those ofelliptical galaxies. Our Local Group model therefore provides a prototypeprogenitor of late--forming elliptical galaxies.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Searches for the permanent electric dipole moments (EDMs) of diamagneticatoms provide powerful probes of CP-violating hadronic and semileptonicinteractions. The theoretical interpretation of such experiments, however,requires careful implementation of a well-known theorem by Schiff that impliesa vanishing net EDM for an atom built entirely from point-like, nonrelativisticconstituents that interact only electrostatically. Any experimental observationof a nonzero atomic EDM would result from corrections to the point-like,nonrelativistic, electrostatic assumption. We reformulate Schiff's theorem atthe operator level and delineate the electronic and nuclear operators whoseatomic matrix elements generate corrections to \"Schiff screening\". We obtain aform for the operator responsible for the leading correction associated withfinite nuclear size -- the so-called \"Schiff moment\" operator -- and observethat it differs from the corresponding operator used in previous Schiff momentcomputations. We show that the more general Schiff moment operator reduces tothe previously employed operator only under certain approximations that are notgenerally justified. We also identify other corrections to Schiff screeningthat may not be included properly in previous theoretical treatments. Wediscuss practical considerations for obtaining a complete computation ofcorrections to Schiff screening in atomic EDM calculations.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "As part of preparations for a southern sky search for faint Milky Way dwarfgalaxy satellites, we report the discovery of a stellar overdensity in theSloan Digital Sky Survey Data Release 5, lying at an angular distance of only1.5 degrees from the recently discovered Bo{\\\"o}tes dwarf. The overdensity wasdetected well above statistical noise by employing a sophisticated data miningalgorithm and does not correspond to any catalogued object. Overlaid isochronesusing stellar population synthesis models show that the color-magnitude diagramof that region has the signature of an old (12 Gyr), metal-poor (${\\rmFe/H}\\approx-2.0$) stellar population at a tentative distance of 60 kpc,evidently the same heliocentric distance as the Bo\\\"otes dwarf. We estimate thenew object to have a total magnitude of $M_{V}\\sim-3.1\\pm1.1$ mag and ahalf-light radius of $r_{h}=4'.1\\pm1'.6$ ($72\\pm28$ pc) placing it in anapparent $40<r_{h}<100$ pc void between globular clusters and dwarf galaxies,occupied only by another recently discovered Milky Way Satellite, ComaBerenices.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present 0.8 to 2.4 micron spectral observations of uranian satellites,obtained at IRTF/SpeX on 17 nights during 2001-2005. The spectra reveal for thefirst time the presence of CO2 ice on the surfaces of Umbriel and Titania, bymeans of 3 narrow absorption bands near 2 microns. Several additional, weakerCO2 ice absorptions have also been detected. No CO2 absorption is seen inOberon spectra, and the strengths of the CO2 ice bands decline withplanetocentric distance from Ariel through Titania. We use the CO2 absorptionsto map the longitudinal distribution of CO2 ice on Ariel, Umbriel, and Titania,showing that it is most abundant on their trailing hemispheres. We also examineH2O ice absorptions in the spectra, finding deeper H2O bands on the leadinghemispheres of Ariel, Umbriel, and Titania, but the opposite pattern on Oberon.Potential mechanisms to produce the observed longitudinal and planetocentricdistributions of the two ices are considered.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "In this paper we derive new expected scaling relations for clusters withgiant radio halos in the framework of the re-acceleration scenario in asimplified, but physically motivated, form, namely: radio power (P_R) vs sizeof the radio emitting region (R_H), and P_R vs total cluster mass (M_H)contained in the emitting region and cluster velocity dispersion (sigma_H) inthis region.  We search for these correlations by analyzing the most recent radio and X-raydata available in the literature for a well known sample of clusters with giantradio halos. In particular we find a good correlation between P_R and R_H and avery tight ``geometrical'' scaling between M_H and R_H. From these correlationsP_R is also expected to scale with M_H and sigma_H and this is confirmed by ouranalysis. We show that all the observed trends can be well reconciled withexpectations in the case of a slight variation of the mean magnetic fieldstrength in the radio halo volume with M_H. A byproduct correlation between R_Hand sigma_H is also found, and can be further tested by optical studies. Inaddition, we find that observationally R_H scales non-linearly with the virialradius of the host cluster, and this immediately means that the fraction of thecluster volume which is radio emitting increases with cluster mass and thusthat the non-thermal component in clusters is not self-similar.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Aims and Methods: We present the results of VLBI observations of nineteenGHz-Peaked-Spectrum (GPS) radio sources at 1.6 GHz. Of them, 15 sources areselected from the Parkes Half Jansky (PHJ) sample (Snellen 2002), 4 others arefrom our previous observation list. We aimed at imaging the structure of GPSsources, searching for Compact Symmetric Objects (CSOs) and studying theabsorption for the convex radio spectra of GPS sources.  Results: We obtained total intensity 1.6 GHz VLBI images of 17 sources forthe first time. Of them, 80% show mini-double-lobe radio structure, indicatingthat they are CSOs or candidates, and their host AGNs could be edge-on to us.This result suggests that there is a high incidence of mini double-lobe sources(or CSOs) in the PHJ sample. The sources J0323+0534, J1135-0021, J1352+0232,J2058+0540, J2123-0112 and J2325-0344 with measured redshift, showingdouble-lobe structure with sizes of <1 kpc, are classified as CSOs. Threesources J1057+0012, J1600-0037 and J1753+2750 are considered as core-jetsources according to their morphologies and flux variability.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We detect a dip of 20-45% in the surface brightness and number counts of NVSSsources smoothed to a few degrees at the location of the WMAP cold spot. Thedip has structure on scales of approximately 1-10 degrees. Together withindependent all-sky wavelet analyses, our results suggest that the dip inextragalactic brightness and number counts and the WMAP cold spot arephysically related, i.e., that the coincidence is neither a statistical anomalynor a WMAP foreground correction problem. If the cold spot does originate fromstructures at modest redshifts, as we suggest, then there is no remaining needfor non-Gaussian processes at the last scattering surface of the CMB to explainthe cold spot. The late integrated Sachs-Wolfe effect, already seenstatistically for NVSS source counts, can now be seen to operate on a singleregion. To create the magnitude and angular size of the WMAP cold spot requiresa ~140 Mpc radius completely empty void at z<=1 along this line of sight. Thisis far outside the current expectations of the concordance cosmology, and addsto the anomalies seen in the CMB.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The Stark shift of the hyperfine coupling constant is investigated for a Pdonor in Si far below the ionization regime in the presence of interfaces usingTight-binding and Band Minima Basis approaches and compared to the recentprecision measurements. The TB electronic structure calculations included over3 million atoms. In contrast to previous effective mass based results, thequadratic Stark coefficient obtained from both theories agrees closely with theexperiments. This work represents the most sensitive and precise comparisonbetween theory and experiment for single donor spin control. It is also shownthat there is a significant linear Stark effect for an impurity near theinterface, whereas, far from the interface, the quadratic Stark effectdominates. Such precise control of single donor spin states is requiredparticularly in quantum computing applications of single donor electronics,which forms the driving motivation of this work.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We analyse star formation in the nuclei of 9 Seyfert galaxies at spatialresolutions down to 0.085arcsec, corresponding to length scales of less than10pc in some objects. Our data were taken mostly with the near infraredadaptive optics integral field spectrograph SINFONI. The stellar light profilestypically have size scales of a few tens of parsecs. In two cases there isunambiguous kinematic evidence for stellar disks on these scales. In thenuclear regions there appear to have been recent - but no longer active -starbursts in the last 10-300Myr. The stellar luminosity is less than a fewpercent of the AGN in the central 10pc, whereas on kiloparsec scales theluminosities are comparable. The surface stellar luminosity density follows asimilar trend in all the objects, increasing steadily at smaller radii up to10^{13}L_sun/kpc^2 in the central few parsecs, where the mass surface densityexceeds 10^4M_sun/pc^2. The intense starbursts were probably Eddington limitedand hence inevitably short-lived, implying that the starbursts occur inmultiple short bursts. The data hint at a delay of 50--100Myr between the onsetof star formation and subsequent fuelling of the black hole. We discuss whetherthis may be a consequence of the role that stellar ejecta could play infuelling the black hole. While a significant mass is ejected by OB winds andsupernovae, their high velocity means that very little of it can be accreted.On the other hand winds from AGB stars ultimately dominate the total mass loss,and they can also be accreted very efficiently because of their slow speeds.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "In a 2002 paper, the authors and Bruner used the new spectrum tmf to obtainsome new nonimmersions of real projective spaces. In this note, wecomplete/correct two oversights in that paper.  The first is to note that in that paper a general nonimmersion result wasstated which yielded new nonimmersions for RP^n with n as small as 48, and yetit was stated there that the first new result occurred when n=1536. Here wegive a simple proof of those overlooked results.  Secondly, we fill in a gap in the proof of the 2002 paper. There it wasclaimed that an axial map f must satisfy f^*(X)=X_1+X_2. We realized recentlythat this is not clear. However, here we show that it is true up multiplicationby a unit in the appropriate ring, and so we retrieve all the nonimmersionresults claimed in the original paper.  Finally, we present a complete determination of tmf^{8*}(RP^\\infty\\timesRP^\\infty) and tmf^*(CP^\\infty\\times CP^\\infty) in positive dimensions.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present a search for the decay B+ -> tau+ nu using 383x10^6 BBbar pairscollected at the Y(4S) resonance with the BABAR detector at the SLAC PEP-IIB-Factory. A sample of events with one reconstructed semileptonic B decay (B--> D0 l nu X)) is selected, and in the recoil a search for B+ -> tau+ nu isperformed. The tau is identified in the following channels: tau+ -> e nu nubar,tau+ -> mu nu nubar, tau+ -> pi+ nu, and tau+ -> pi+ pi0 nu. We measure abranching fraction of B(B+ -> tau+ nu)=(0.9 +- 0.6(stat.) +- 0.1(syst.)) x10^-4. In the absence of a significant signal, we calculate an upper limit atthe 90% confidence level of B(B+ -> tau+ nu) < 1.7 x 10^-4. We calculate theproduct of the B meson decay constant f_B and |V_ub| to be f_B x |V_ub| =(7.2^{+2.0}_{-2.8}(stat.) +- 0.2 (syst.)) x 10^-4 GeV.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "This paper presents a hybrid approach to spatial indexing of two dimensionaldata. It sheds new light on the age old problem by thinking of the traditionalalgorithms as working with images. Inspiration is drawn from an analogoussituation that is found in machine and human vision. Image processingtechniques are used to assist in the spatial indexing of the data. A fixed gridapproach is used and bins with too many records are sub-divided hierarchically.Search queries are pre-computed for bins that do not contain any data records.This has the effect of dividing the search space up into non rectangularregions which are based on the spatial properties of the data. The bucketingquad tree can be considered as an image with a resolution of two by two foreach layer. The results show that this method performs better than the quadtree if there are more divisions per layer. This confirms our suspicions thatthe algorithm works better if it gets to look at the data with higherresolution images. An elegant class structure is developed where theimplementation of concrete spatial indexes for a particular data type merelyrelies on rendering the data onto an image.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present the first strong lensing study of the mass distribution in thecluster MS 2053-04 based on HST archive data. This massive, X-ray luminouscluster has a redshift z=0.583, and it is composed of two structures that aregravitationally bound to each other. The cluster has one multiply imaged systemconstituted by a double gravitational arc.  We have performed a parametric strong lensing mass reconstruction using NFWdensity profiles to model the cluster potential. We also included perturbationsfrom 23 galaxies, modeled like elliptical singular isothermal sphere, that areapproximately within 1'x1' around the cluster center. These galaxies wereconstrained in both the geometric and dynamical parameters with observationaldata. Our analysis predicts a third image which is slightly demagnified. Wefound a candidate for this counter-image near the expected position and withthe same F702W-F814W colors as the gravitational arcs in the cluster. Theresults from the strong lensing model shows the complex structure in thiscluster, the asymmetry and the elongation in the mass distribution, and areconsistent with previous spectrophotometric results that indicate that thecluster has a bimodal mass distribution. Finally, the derived mass profile wasused to estimate the mass within the arcs and for comparison with X-rayestimates.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "In the last decade evidence has accumulated that small domains of 50-700 nmin diameter are located in the exoplasmic leaflet of the plasma membrane. Mostof these domains supposedly consist of specific sets of lipids and proteins,and are believed to coordinate signal transduction cascades. Whether similardomains are also present in the cytoplasmic leaflet of the plasma membrane isunclear so far. To investigate the presence of cytoplasmic leaflet domains, theH-Ras membrane-targeting sequence was fused to the C-terminus of the enhancedyellow fluorescent protein. Using single-molecule fluorescence microscopy,trajectories of individual molecules diffusing in the cytoplasmic leaflet ofthe plasma membrane were recorded. From these trajectories, the diffusion ofindividual membrane-anchored enhanced yellow fluorescent protein molecules wasstudied in live cells on timescales from 5 to 200 ms. The results show that thediffusion of 30-40% of the molecules is constrained in domains with a typicalsize of 200 nm. Neither breakdown of actin nor cholesterol extraction changedthe domain characteristics significantly, indicating that the observed domainsmay not be related to the membrane domains identified so far.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We investigate dynamical properties of bright solitons with a finitebackground in the F=1 spinor Bose-Einstein condensate (BEC), based on anintegrable spinor model which is equivalent to the matrix nonlinearSchr\\\"{o}dinger equation with a self-focusing nonlineality. We apply theinverse scattering method formulated for nonvanishing boundary conditions. Theresulting soliton solutions can be regarded as a generalization of those undervanishing boundary conditions. One-soliton solutions are derived in an explicitmanner. According to the behaviors at the infinity, they are classified intotwo kinds, domain-wall (DW) type and phase-shift (PS) type. The DW-type impliesthe ferromagnetic state with nonzero total spin and the PS-type implies thepolar state, where the total spin amounts to zero. We also discuss two-solitoncollisions. In particular, the spin-mixing phenomenon is confirmed in acollision involving the DW-type. The results are consistent with those of theprevious studies for bright solitons under vanishing boundary conditions anddark solitons. As a result, we establish the robustness and the usefulness ofthe multiple matter-wave solitons in the spinor BECs.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present the results of realistic N-body modelling of massive star clustersin the Magellanic Clouds, aimed at investigating a dynamical origin for theradius-age trend observed in these systems. We find that stellar-mass blackholes, formed in the supernova explosions of the most massive cluster stars,can constitute a dynamically important population. If a significant number ofblack holes are retained (here we assume complete retention), these objectsrapidly form a dense core where interactions are common, resulting in thescattering of black holes into the cluster halo, and the ejection of blackholes from the cluster. These two processes heat the stellar component,resulting in prolonged core expansion of a magnitude matching the observations.Significant core evolution is also observed in Magellanic Cloud clusters atearly times. We find that this does not result from the action of black holes,but can be reproduced by the effects of mass-loss due to rapid stellarevolution in a primordially mass segregated cluster.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Heteroepitaxial self-assembled quantum dots (SAQDs) will allow breakthroughsin electronics and optoelectronics. SAQDs are a result of Stranski-Krastanowgrowth whereby a growing planar film becomes unstable after an initial wettinglayer is formed. Common systems are Ge$_{x}$Si$_{1-x}$/Si andIn$_{x}$Ga$_{1-x}$As/GaAs. For applications, SAQD arrays need to be ordered.The role of crystal anisotropy, random initial conditions and thermalfluctuations in influencing SAQD order during early stages of SAQD formation isstudied through a simple stochastic model of surface diffusion. Surfacediffusion is analyzed through a linear and perturbatively nonlinear analysis.The role of crystal anisotropy in enhancing SAQD order is elucidated. It isalso found that SAQD order is enhanced when the deposited film is allowed toevolve at heights near the critical wetting surface height that marks the onsetof non-planar film growth.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The Cosmic Far-Infrared Background (CFIRB) contains information about thenumber and distribution of contributing sources and thus gives us an importantkey to understand the evolution of galaxies. Using a confusion study to set afundamental limit to the observations, we investigate the potential to explorethe CFIRB with AKARI/FIS deep observations. The Far-Infrared Surveyor (FIS) isone of the focal-plane instruments on the AKARI (formerly known as ASTRO-F)satellite, which was launched in early 2006. Based upon source distributionmodels assuming three different cosmological evolutionary scenarios (noevolution, weak evolution, and strong evolution), an extensive model fordiffuse emission from infrared cirrus, and instrumental noise estimates, wepresent a comprehensive analysis for the determination of the confusion levelsfor deep far-infrared observations. We use our derived sensitivities to suggestthe best observational strategy for the AKARI/FIS mission to detect the CFIRBfluctuations. If the source distribution follows the evolutionary models,observations will be mostly limited by source confusion. We find that we willbe able to detect the CFIRB fluctuations and that these will in turn provideinformation to discriminate between the evolutionary scenarios of galaxies inmost low-to-medium cirrus regions.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Prominent ethical and policy issues such as affirmative action and femaleenrollment in science and engineering revolve around the idea that diversity isgood. However, even though diversity is an ambiguous concept, a precisedefinition is seldom provided. We show that diversity may be construed as afactual description, a craving for symmetry, an intrinsic good, an instrumentalgood, a symptom, or a side effect. These acceptions differ vastly in theirnature and properties. The first one cannot lead to any action and the secondone is mistaken. Diversity as intrinsic good is a mere opinion, which cannot beconcretely applied; moreover, the most commonly invoked forms of diversity(sexual and racial) are not intrinsically good. On the other hand, diversity asinstrumental good can be evaluated empirically and can give rise to policies,but these may be very weak. Finally, symptoms and side effects are not actuallyabout diversity. We consider the example of female enrollment in science andengineering, interpreting the various arguments found in the literature inlight of this polysemy.  Keywords: ethics, policy, higher education, female students, minoritystudents, affirmative action", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Electromechanical coupling is ubiquitous in biological systems with examplesranging from simple piezoelectricity in calcified and connective tissues tovoltage-gated ion channels, energy storage in mitochondria, andelectromechanical activity in cardiac myocytes and outer hair cell stereocilia.Piezoresponse force microscopy (PFM) has originally emerged as a technique tostudy electromechanical phenomena in ferroelectric materials, and in recentyears, has been employed to study a broad range of non-ferroelectric polarmaterials, including piezoelectric biomaterials. At the same time, thetechnique has been extended from ambient to liquid imaging on modelferroelectric systems. Here, we present results on local electromechanicalprobing of several model cellular and biomolecular systems, including insulinand lysozyme amyloid fibrils, breast adenocarcinoma cells, andbacteriorhodopsin in a liquid environment. The specific features of SPMoperation in liquid are delineated and bottlenecks on the route towardsnanometer-resolution electromechanical imaging of biological systems areidentified.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Recently, much research has been carried out on Hamiltonians that are notHermitian but are symmetric under space-time reflection, that is, Hamiltoniansthat exhibit PT symmetry. Investigations of the Sturm-Liouville eigenvalueproblem associated with such Hamiltonians have shown that in many cases theentire energy spectrum is real and positive and that the eigenfunctions form anorthogonal and complete basis. Furthermore, the quantum theories determined bysuch Hamiltonians have been shown to be consistent in the sense that theprobabilities are positive and the dynamical trajectories are unitary. However,the geometrical structures that underlie quantum theories formulated in termsof such Hamiltonians have hitherto not been fully understood. This paperstudies in detail the geometric properties of a Hilbert space endowed with aparity structure and analyses the characteristics of a PT-symmetric Hamiltonianand its eigenstates. A canonical relationship between a PT-symmetric operatorand a Hermitian operator is established. It is shown that the quadratic formcorresponding to the parity operator, in particular, gives rise to a naturalpartition of the Hilbert space into two halves corresponding to states havingpositive and negative PT norm. The indefiniteness of the norm can becircumvented by introducing a symmetry operator C that defines a positivedefinite inner product by means of a CPT conjugation operation.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Observations of stellar activity cycles provide an opportunity to studymagnetic dynamos under many different physical conditions. Space-basedasteroseismology missions will soon yield useful constraints on the interiorconditions that nurture such magnetic cycles, and will be sensitive enough todetect shifts in the oscillation frequencies due to the magnetic variations. Wederive a method for predicting these shifts from changes in the Mg II activityindex by scaling from solar data. We demonstrate this technique on thesolar-type subgiant beta Hyi, using archival International Ultraviolet Explorerspectra and two epochs of ground-based asteroseismic observations. We findqualitative evidence of the expected frequency shifts and predict the optimaltiming for future asteroseismic observations of this star.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We report on the measurement of element-specific magnetic resonance spectraat gigahertz frequencies using x-ray magnetic circular dichroism (XMCD). Weinvestigate the ferrimagnetic precession of Gd and Fe ions in Gd-substitutedYttrium Iron Garnet, showing that the resonant field and linewidth of Gdprecisely coincide with Fe up to the nonlinear regime of parametricexcitations. The opposite sign of the Gd x-ray magnetic resonance signal withrespect to Fe is consistent with dynamic antiferromagnetic alignment of the twoionic species. Further, we investigate a bilayer metal film,Ni$_{80}$Fe$_{20}$(5 nm)/Ni(50 nm), where the coupled resonance modes of Ni andNi$_{80}$Fe$_{20}$ are separately resolved, revealing shifts in the resonancefields of individual layers but no mutual driving effects. Energy-dependentdynamic XMCD measurements are introduced, combining x-ray absorption andmagnetic resonance spectroscopies.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We use the Barnard 68 dark globule as a test case for a spherically symmetricPDR model exposed to low-UV radiation fields. With a roughly sphericalmorphology and an accurately determined density profile, Barnard 68 is idealfor this purpose. The processes governing the energy balance in the cloudsurface are studied in detail. We compare the spherically symmetric PDR modelby Stoerzer, Stutzki & Sternberg (1996) to observations of the three lowestrotational transitions of 12CO, 13CO J = 2-1 and J = 3-2 as well as the [CI]3P_1-3P_0 fine structure transition. We study the role of Polycyclic AromaticHydrocarbons (PAHs) in the chemical network of the PDR model and consider theimpact of depletion as well as of a variation of the external FUV field. Wefind it difficult to simultaneously model the observed 12CO and 13CO emission.The 12CO and [CI] emission can be explained by a PDR model with a external FUVfield of 1-0.75 chi_0, but this model fails to reproduce the observed 13CO by afactor of ~2. Adding PAHs to the chemical network increases the [CI] emissionby 50% in our model but makes [CII] very faint. CO depletion only slightlyreduces the 12CO and 13CO line intensity (by <10% and <20%, respectively).Predictions for the [CII] 2P_3/2-2P_1/2, [CI] 3P_2-3P_1 and 12CO J= 5-4 and 4-3transitions are presented. This allows a test of our model with futureobservations (APEX, NANTEN2, HERSCHEL, SOFIA).", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We have investigated the influence of nuclear parameters such as black hole(BH) mass and photoionizing luminosity on the FRI/FRII transition in a sampleof nearby (z<0.2) 3CR radio galaxies. The sample was observed withmedium-resolution, optical spectroscopy and contains some galaxies withunpublished velocity dispersion measurements and emission-line fluxes. Measuredvelocity dispersions are 130-340 km/s with a mean of 216 km/s. Converting to BHmass, we find that the BH mass distribution is identical for FRIs and FRIIs,with a mean of approximately 2.5x10^8 Msun. We convert [OII] and [OIII]emission-line luminosities to photoionizing luminosity under the assumptionthat the gas is ionized by the nuclear UV continuum. Most of the galaxies withFRI morphology and/or low-excitation emission-line spectra have progressivelylower BH masses at lower photoionizing (and jet) luminosities. This agrees withthe Ledlow-Owen relation which states that the radio luminosity at the FRI/FRIItransition depends on the optical luminosity of the host, L_radio ~L_optical^1.8, because both L_radio and L_optical relate to AGN nuclearparameters. When recasting the Ledlow-Owen relation into BH mass versusphotoionizing and jet luminosity, we find that the recasted relation describesthe sample quite well. The FRI/FRII transition occurs at approximately an orderof magnitude lower luminosity relative to the Eddington luminosity than thesoft-to-hard transition in X-ray binaries. This difference is consistent withthe Ledlow-Owen relation, which predicts a weak BH mass dependence in thetransition luminosity. We conclude that the FRI/FRII dichotomy is caused by acombination of external and nuclear factors, with the latter dominating.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Quantum computers have the capability of out-performing their classicalcounterparts for certain computational problems. Several scalable quantumcomputing architectures have been proposed. An attractive architecture is alarge set of physically independant qubits, arranged in three spatial regionswhere (i) the initialized qubits are stored in a register, (ii) two qubits arebrought together to realize a gate, and (iii) the readout of the qubits isperformed. For a neutral atom-based architecture, a natural way to connectthese regions is to use optical tweezers to move qubits within the system. Inthis letter we demonstrate the coherent transport of a qubit, encoded on anatom trapped in a sub-micron tweezer, over a distance typical of the separationbetween atoms in an array of optical traps. Furthermore, we transfer a qubitbetween two tweezers, and show that this manipulation also preserves thecoherence of the qubit.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We characterize the molecular environment of candidate massive young stellarobjects (MYSOs) signposted by methanol masers. Single pixel observations of 10transitions of HCO^+, CO and CS isotopomers were carried out, using the IRAM30m telescope. We studied a sample of 28 targets for which the 6.7GHz maseremission positions are known with a sub-arcsecond accuracy. The systemicvelocity inferred from the optically thin lines agrees within 3km/s with thecentral velocity of the maser emission for most of the sources. About 64% ofthe sources show line wings in one or more transitions of CO, HCO^+ and CSspecies, indicating the presence of molecular outflows. Comparison of thewidths of line wings and methanol maser emission suggests that the 6.7GHz maserline traces the environment of MYSO of various kinematic regimes. Thereforeconditions conducive for the methanol maser can exist in the inner parts ofmolecular clouds or circumstellar discs as well as in the outer partsassociated with molecular outflows. Calculations of the physical conditionsbased on the CO and HCO^+ lines and the CS line intensity ratios refine theinput parameters for maser models.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present SEST observations of the molecular environment ahead of thesouthern Herbig-Haro object 188 (HH188), associated with the low-mass protostarRe4 IRS. We have also used the SuperCosmos Halpha survey to search for Halphaemission associated with the Re4 IRS - HH188 region. The aim of the presentwork is to study the properties of the molecular gas and to better characterizethis southern star forming region. We mapped the HCO+ 3-2 and H13CO+ 1-0emission around the YSO and took spectra of the CH3OH 2(0)-1(0)A+ and2(-1)-1(-1)E and SO 6(5)-5(4) towards the central source. Column densities arederived and different scenarios are considered to explain the origin of themolecular emission. HCO+ arises from a relatively compact region around theYSO; however, its peak emission is displaced to the south following the outflowdirection. Our chemical analysis indicates that a plausible scenario is thatmost of the emission arises from the cold, illuminated dense gas ahead of theHH188 object. We have also found that HH188, a high excitation object, seems tobe part of a parsec scale and highly collimated HH system. Re4 IRS is probablya binary protostellar system, in the late Class 0 or Class I phase. One of theprotostars, invisible in the near-IR, seems to power the HH188 system.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The effect of Ge substitution for Si in SmMMn2Si2-xGex compounds has beenstudied. The Sm ordering temperature is found to be much larger in the compoundwith x=2, as compared to the compounds with x=0 and 1. The increase in theintra layer Mn-Mn distance is found to be responsible for this increase. Amongthese three compounds, SmMn2Ge2 is found to show re-entrant ferromagnetism atlow temperatures. The magnetic contribution to the heat capacity has been foundin all the three compounds. The splitting of the ground state multiplet hasbeen estimated by fitting the magnetic part of the heat capacity data using theSchottky formula. The isothermal magnetic entropy change is found to remain thesame for x=0 and 1, but decrease in the compound with x=2, though the nature ofmagnetic transition changes from second order to first order, as x is increasedfrom 0 to 2. The electrical resistivity increases with Ge concentration. Theexcess resistivity in the antiferromagnetic region has been calculated.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Bigravity is a natural arena where a non-linear theory of massive gravity canbe formulated. If the interaction between the metrics $f$ and $g$ isnon-derivative, spherically symmetric exact solutions can be found. At largedistances from the origin, these are generically Lorentz-breaking bi-flatsolutions (provided that the corresponding vacuum energies are adjustedappropriately). The spectrum of linearized perturbations around suchbackgrounds contains a massless as well as a massive graviton, with {\\em two}physical polarizations each. There are no propagating vectors or scalars, andthe theory is ghost free (as happens with certain massive gravities withexplicit breaking of Lorentz invariance). At the linearized level, correctionsto GR are proportional to the square of the graviton mass, and so there is novDVZ discontinuity. Surprisingly, the solution of linear theory for a staticspherically symmetric source does {\\em not} agree with the linearization of anyof the known exact solutions. The latter coincide with the standardSchwarzschild-(A)dS solutions of General Relativity, with no corrections atall. Another interesting class of solutions is obtained where $f$ and $g$ areproportional to each other. The case of bi-de Sitter solutions is analyzed insome detail.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We investigate the generation of quantum operations for one-qubit systemsunder classical noise with 1/f^\\alpha power spectrum, where 2>\\alpha > 0. Wepresent an efficient way to approximate the noise with a discrete multi-stateMarkovian fluctuator. With this method, the average temporal evolution of thequbit density matrix under 1/f^\\alpha noise can be feasibly determined fromrecently derived deterministic master equations. We obtain qubit operationssuch as quantum memory and the NOT}gate to high fidelity by a gradient basedoptimization algorithm. For the NOT gate, the computed fidelities arequalitatively similar to those obtained earlier for random telegraph noise. Inthe case of quantum memory however, we observe a nonmonotonic dependency of thefidelity on the operation time, yielding a natural access rate of the memory.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The structure of three laminar premixed rich flames has been investigated: apure methane flame and two methane flames doped by allene and propyne,respectively. The gases of the three flames contain 20.9% (molar) of methaneand 33.4% of oxygen, corresponding to an equivalence ratio of 1.25 for the puremethane flame. In both doped flames, 2.49% of C3H4 was added, corresponding toa ratio C3H4/CH4 of 12% and an equivalence ratio of 1.55. The three flames havebeen stabilized on a burner at a pressure of 6.7 kPa using argon as dilutant,with a gas velocity at the burner of 36 cm/s at 333 K. The concentrationprofiles of stable species were measured by gas chromatography after samplingwith a quartz microprobe. Quantified species included carbon monoxide anddioxide, methane, oxygen, hydrogen, ethane, ethylene, acetylene, propyne,allene, propene, propane, 1,2-butadiene, 1,3-butadiene, 1-butene, isobutene,1-butyne, vinylacetylene, and benzene. The temperature was measured using aPtRh (6%)-PtRh (30%) thermocouple settled inside the enclosure and ranged from700 K close to the burner up to 1850 K. In order to model these new results,some improvements have been made to a mechanism previously developed in ourlaboratory for the reactions of C3-C4 unsaturated hydrocarbons. The mainreaction pathways of consumption of allene and propyne and of formation of C6aromatic species have been derived from flow rate analyses.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "According to extensive experimental findings, the Ginzburg temperature$t_{G}$ for ionic fluids differs substantially from that of nonionic fluids[Schr\\\"oer W., Weig\\\"{a}rtner H. 2004 {\\it Pure Appl. Chem.} {\\bf 76} 19]. Atheoretical investigation of this outcome is proposed here by a mean fieldanalysis of the interplay of short and long range interactions on the value of$t_{G}$. We consider a quite general continuous charge-asymmetric model made ofcharged hard spheres with additional short-range interactions (withoutelectrostatic interactions the model belongs to the same universality class asthe 3D Ising model). The effective Landau-Ginzburg Hamiltonian of the fullsystem near its gas-liquid critical point is derived from which the Ginzburgtemperature is calculated as a function of the ionicity. The results obtainedin this way for $t_{G}$ are in good qualitative and sufficient quantitativeagreement with available experimental data.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We investigate the optical properties of one-dimensional (1D) dimerized Mottinsulators using the 1D dimerized extended Hubbard model. Numericalcalculations and a perturbative analysis from the decoupled-dimer limit clarifythat there are three relevant classes of charge-transfer (CT) states generatedby photoexcitation: interdimer CT unbound states, interdimer CT exciton states,and intradimer CT exciton states. This classification is applied tounderstanding the optical properties of an organic molecular material,1,3,5-trithia-2,4,6-triazapentalenyl (TTTA), which is known for itsphotoinduced transition from the dimerized spin-singlet phase to the regularparamagnetic phase. We conclude that the lowest photoexcited state of TTTA isthe interdimer CT exciton state and the second lowest state is the intradimerCT exciton state.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Mn3V2O8 is a magnetic system in which S = 5/2 Mn2+ is found in the kagomestaircase lattice. Here we report the magnetic phase diagram for temperaturesabove 2 K and applied magnetic fields below 9 T, characterized by measurementsof the magnetization and specific heat with field along the three uniquelattice directions. At low applied magnetic fields, the system first ordersmagnetically below Tm1 ~ 21 K, and then shows a second magnetic phasetransition at Tm2 ~ 15 K. In addition, a phase transition that is apparent inspecific heat but not seen in magnetization is found for all three appliedfield orientations, converging towards Tm2 as H -> 0. The magnetic behavior ishighly anisotropic, with critical fields for magnetic phase boundaries muchhigher when the field is applied perpendicular to the Kagome staircase planethan when applied in-plane. The field-temperature (H - T) phase diagrams arequite rich, with 7 distinct phases observed.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "A k-query Locally Decodable Code (LDC) encodes an n-bit message x as an N-bitcodeword C(x), such that one can probabilistically recover any bit x_i of themessage by querying only k bits of the codeword C(x), even after some constantfraction of codeword bits has been corrupted. The major goal of LDC relatedresearch is to establish the optimal trade-off between length and querycomplexity of such codes.  Recently [Y] introduced a novel technique for constructing locally decodablecodes and vastly improved the upper bounds for code length. The technique isbased on Mersenne primes. In this paper we extend the work of [Y] and arguethat further progress via these methods is tied to progress on an old numbertheory question regarding the size of the largest prime factors of Mersennenumbers.  Specifically, we show that every Mersenne number m=2^t-1 that has a primefactor p>m^\\gamma yields a family of k(\\gamma)-query locally decodable codes oflength Exp(n^{1/t}). Conversely, if for some fixed k and all \\epsilon > 0 onecan use the technique of [Y] to obtain a family of k-query LDCs of lengthExp(n^\\epsilon); then infinitely many Mersenne numbers have prime factors argerthan known currently.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Density-functional theory has been applied to investigate systematics ofsodium clusters Na_n in the size range of n= 39-55. A clear evolutionary trendin the growth of their ground-state geometries emerges. The clusters at thebeginning of the series (n=39-43) are symmetric and have partial icosahedral(two-shell) structure. The growth then goes through a series of disorderedclusters (n=44-52) where the icosahedral core is lost. However, for n>52 athree shell icosahedral structure emerges. This change in the nature of thegeometry is abrupt. In addition, density-functional molecular dynamics has beenused to calculate the specific heat curves for the representative sizes n= 43,45, 48 and 52. These results along with already available thermodynamiccalculations for n= 40, 50, and 55 enable us to carry out a detailed comparisonof the heat capacity curves with their respective geometries for the entireseries. Our results clearly bring out strong correlation between the evolutionof the geometries and the nature of the shape of the heat capacities. Theresults also firmly establish the size-sensitive nature of the heat capacitiesin sodium clusters.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The stationary hydrodynamic equations for the transonic accretion disks andflows around rotating black holes are presented by using the Kerr-Schildcoordinate where there is no coordinate singularity at the event horizon. Weuse two types of the causal viscosity prescription, and the boundary conditionsfor the transonic accretion flows are given at the sonic point. For one type ofthe causal viscosity prescription we also add the boundary conditions at theviscous point where the accreting radial velocity is nearly equal to theviscous diffusion velocity. Based on the formalism for the transonic accretiondisks, after we present the calculation method of the transonic solutions, thehorizon-penetrating transonic solutions which smoothly pass the event horizonare calculated for several types of the accretion flow models: the idealisothermal flows, the ideal and the viscous polytropic flows, the advectiondominated accretion flows (ADAFs) with the relativistic equation of state, theadiabatic accretion disks, the standard accretion disks, the supercriticalaccretion disks. These solutions are obtained for both non-rotating androtating black holes. The calculated accretion flows plunge into black holewith finite three velocity smaller than the speed of light even at the eventhorizon or inside the horizon, and the angular velocities of the accretion flowat the horizon are generally different from the angular velocity of theframe-dragging due to the black hole's rotation. These features contrast to theresults obtained by using the Boyer-Lindquist coordinate with the coordinatesingularity at the horizon.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Phenomenologically viable and interesting regions of parameter space in theminimal super-gravity (mSUGRA) model with small $m_0$ and small $m_{1/2}$consistent with the WMAP data on dark matter relic density and the bound on themass of the lightest Higgs scalar $ m_h>$ 114 GeV from LEP2 open up if therather adhoc assumption $A_0$=0, where $A_0$ is the common trilinear softbreaking parameter, employed in most of the existing analyses is relaxed. Sincethis region corresponds to relatively light squarks and gluinos which arelikely to be probed extensively in the very early stages of the LHCexperiments, the consequences of moderate or large negative values of $A_0$ areexamined in detail. We find that in this region several processes includinglightest supersymmetric particle (LSP) pair annihilation, LSP - lighter tauslepton (${\\tilde \\tau}_1$) coannihilation and LSP - lighter top squark(${\\tilde t}_1$) coannihilation contribute to the observed dark matter relicdensity. %\\sout{The possibility that a relic density producing ${\\tilde t}_1$can be %observed at the current experiments at the Tevatron is wide open.} Thepossibility that a ${\\tilde t}_1$ that can participate in coannihilation withthe lightest neutralino to satisfy the WMAP bound on relic density and at thesame time be observed at the current experiments at the Tevatron is wide open.At the LHC a large number of squark - gluino events lead to a very distinctivesemi-inclusive signature $\\tau^\\pm$+X$_\\tau$ (anything without a tau lepton)with a characteristic size much larger than $e^\\pm$+X$_e$ or $\\mu^\\pm$+X$_\\mu$events.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "It has been shown recently by Kapustin and Tomasiello that the mathematicalnotion of Hamiltonian actions on twisted generalized K\\\"ahler manifolds is inperfect agreement with the physical notion of general $(2,2)$ gauged sigmamodels with three-form fluxes. In this article, we study the twistedequivariant cohomology theory of Hamiltonian actions on $H$-twisted generalizedcomplex manifolds. If the manifold satisfies the$\\bar{\\partial}\\partial$-lemma, we establish the equivariant formality theorem.If in addition, the manifold satisfies the generalized K\\\"ahler condition, weprove the Kirwan injectivity in this setting. We then consider the Hamiltonianaction of a torus on an $H$-twisted generalized Calabi-Yau manifold and extendto this case the Duistermaat-Heckman theorem for the push-forward measure.  As a side result, we show in this paper that the generalized K\\\"ahlerquotient of a generalized K\\\"ahler vector space can never have a(cohomologically) non-trivial twisting. This gives a negative answer to aquestion asked by physicists whether one can construct $(2,2)$ gauged linearsigma models with non-trivial fluxes.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We show numerically that in a binary system of Yukawa particles, a dispersitydriven disordering transition occurs. In the presence of quenched disorder thisdisordering transition coincides with a marked increase in the depinningthreshold, known as a peak effect. We find that the addition of poorly pinnedparticles can increase the overall pinning in the sample by increasing theamount of topological disorder present. If the quenched disorder is strongenough to create a significant amount of topological disorder in themonodisperse system, addition of a poorly pinned species generates furtherdisorder but does not produce a peak in the depinning force. Our resultsindicate that for binary mixtures, optimal pinning occurs for topologicaldefect fraction densities of 0.2 to 0.25. For defect densities below thisrange, the system retains orientational order. We determine the effect of thepinning density, strength, and radius on the depinning peak and find that thepeak effect is more pronounced in weakly pinning systems.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present photometric detections of dust emission at 850 and 450 micronaround the pre-main sequence M1 dwarf TWA 7 using the SCUBA camera on the JamesClerk Maxwell Telescope. These data confirm the presence of a cold dust diskaround TWA 7, a member of the TW Hydrae Association. Based on the 850 micronflux, we estimate the mass of the disk to be 18 lunar masses (0.2 Earth masses)assuming a mass opacity of 1.7 cm^2/g with a temperature of 45 K. This makesthe TWA 7 disk (d=55 pc) an order of magnitude more massive than the diskreported around AU Microscopii (GL 803), the closest (9.9 pc) debris diskdetected around an M dwarf. This is consistent with TWA 7 being slightlyyounger than AU Mic. We find that the mid-IR and submillimeter data require thedisk to be comprised of dust at a range of temperatures. A model in which thedust is at a single radius from the star, with a range of temperaturesaccording to grain size, is as effective at fitting the emission spectrum as amodel in which the dust is of uniform size, but has a range of temperaturesaccording to distance. We discuss this disk in the context of known disks inthe TW Hydrae Association and around low-mass stars; a comparison of masses ofdisks in the TWA reveals no trend in mass or evolutionary state (gas-rich vs.debris) as a function of spectral type.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Integral formulae for polynomial solutions of the quantumKnizhnik-Zamolodchikov equations associated with the R-matrix of the six-vertexmodel are considered. It is proved that when the deformation parameter q isequal to e^{+- 2 pi i/3} and the number of vertical lines of the lattice isodd, the solution under consideration is an eigenvector of the inhomogeneoustransfer matrix of the six-vertex model. In the homogeneous limit it is aground state eigenvector of the antiferromagnetic XXZ spin chain with theanisotropy parameter Delta equal to -1/2 and odd number of sites. The obtainedintegral representations for the components of this eigenvector allow to provesome conjectures on its properties formulated earlier. A new statement relatingthe ground state components of XXZ spin chains and Temperley-Lieb loop modelsis formulated and proved.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We analyze the effect of variation of fundamental couplings and mass scaleson primordial nucleosynthesis in a systematic way. The first step establishesthe response of primordial element abundances to the variation of a largenumber of nuclear physics parameters, including nuclear binding energies. Wefind a strong influence of the n-p mass difference (for the 4He abundance), ofthe nucleon mass (for deuterium) and of A=3,4,7 binding energies (for 3He, 6Liand 7Li). A second step relates the nuclear parameters to the parameters of theStandard Model of particle physics. The deuterium, and, above all, 7Liabundances depend strongly on the average light quark mass hat{m} \\equiv(m_u+m_d)/2. We calculate the behaviour of abundances when variations offundamental parameters obey relations arising from grand unification. We alsodiscuss the possibility of a substantial shift in the lithium abundance whilethe deuterium and 4He abundances are only weakly affected.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We investigate colour selection techniques for high redshift galaxies in theUKIDSS Ultra Deep Survey Early Data Release (UDS EDR). Combined with very deepSubaru optical photometry, the depth (K_AB = 22.5) and area (0.62 deg^2) of theUDS EDR allows us to investigate optical/near-IR selection using a large sampleof over 30,000 objects. By using the B-z, z-K colour-colour diagram (the BzKtechnique) we identify over 7500 candidate galaxies at z > 1.4, which can befurther separated into passive and starforming systems (pBzK and sBzKrespectively). Our unique sample allows us to identify a new feature notpreviously seen in BzK diagrams, consistent with the passively evolving trackof early type galaxies at z < 1.4. We also compare the BzK technique with theR-K colour selection of Extremely Red Objects (EROs) and the J-K selection ofDistant Red Galaxies (DRGs), and quantify the overlap between thesepopulations. We find that the majority of DRGs, at these relatively brightmagnitudes are also EROs. Since previous studies have found that DRGs at thesemagnitudes have redshifts of z ~ 1 we determine that these DRG/ERO galaxieshave SEDs consistent with being dusty star-forming galaxies or AGN at z < 2.Finally we observe a flattening in the number counts of pBzK galaxies, similarto other studies, which may indicate that we are sampling the luminosityfunction of passive z > 1 galaxies over a narrow redshift range.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "In this manuscript we investigate the capabilities of the Discrete DipoleApproximation (DDA) to simulate scattering from particles that are much largerthan the wavelength of the incident light, and describe an optimized publiclyavailable DDA computer program that processes the large number of dipolesrequired for such simulations. Numerical simulations of light scattering byspheres with size parameters x up to 160 and 40 for refractive index m=1.05 and2 respectively are presented and compared with exact results of the Mie theory.Errors of both integral and angle-resolved scattering quantities generallyincrease with m and show no systematic dependence on x. Computational timesincrease steeply with both x and m, reaching values of more than 2 weeks on acluster of 64 processors. The main distinctive feature of the computer programis the ability to parallelize a single DDA simulation over a cluster ofcomputers, which allows it to simulate light scattering by very largeparticles, like the ones that are considered in this manuscript. Currentlimitations and possible ways for improvement are discussed.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "This article surveys many standard results about the braid group withemphasis on simplifying the usual algebraic proofs.  We use van der Waerden's trick to illuminate the Artin-Magnus proof of theclassic presentation of the algebraic mapping-class group of a punctured disc.  We give a simple, new proof of the Dehornoy-Larue braid-group trichotomy,and, hence, recover the Dehornoy right-ordering of the braid group.  We then turn to the Birman-Hilden theorem concerning braid-group actions onfree products of cyclic groups, and the consequences derived by Perron-Vannier,and the connections with the Wada representations. We recall the very simpleCrisp-Paris proof of the Birman-Hilden theorem that uses the Larue-Shpilraintechnique. Studying ends of free groups permits a deeper understanding of thebraid group; this gives us a generalization of the Birman-Hilden theorem.Studying Jordan curves in the punctured disc permits a still deeperunderstanding of the braid group; this gave Larue, in his PhD thesis,correspondingly deeper results, and, in an appendix, we recall the essence ofLarue's thesis, giving simpler combinatorial proofs.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present a mathematically justifiable, computationally simple, sampleeigenvalue based procedure for estimating the number of high-dimensionalsignals in white noise using relatively few samples. The main motivation forconsidering a sample eigenvalue based scheme is the computational simplicityand the robustness to eigenvector modelling errors which are can adverselyimpact the performance of estimators that exploit information in the sampleeigenvectors.  There is, however, a price we pay by discarding the information in the sampleeigenvectors; we highlight a fundamental asymptotic limit of sample eigenvaluebased detection of weak/closely spaced high-dimensional signals from a limitedsample size. This motivates our heuristic definition of the effective number ofidentifiable signals which is equal to the number of \"signal\" eigenvalues ofthe population covariance matrix which exceed the noise variance by a factorstrictly greater than 1+sqrt(Dimensionality of the system/Sample size). Thefundamental asymptotic limit brings into sharp focus why, when there are toofew samples available so that the effective number of signals is less than theactual number of signals, underestimation of the model order is unavoidable (inan asymptotic sense) when using any sample eigenvalue based detection scheme,including the one proposed herein. The analysis reveals why adding more sensorscan only exacerbate the situation. Numerical simulations are used todemonstrate that the proposed estimator consistently estimates the true numberof signals in the dimension fixed, large sample size limit and the effectivenumber of identifiable signals in the large dimension, large sample size limit.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We study Batch Processor-Sharing (BPS) queuing model with hyper-exponentialservice time distribution and Poisson batch arrival process. One of the maingoals to study BPS is the possibility of its application in size-basedscheduling, which is used in differentiation between Short and Long flows inthe Internet. In the case of hyper-exponential service time distribution wefind an analytical expression of the expected conditional response time for theBPS queue. We show, that the expected conditional response time is a concavefunction of the service time. We apply the received results to the Two LevelProcessor-Sharing (TLPS) model with hyper-exponential service time distributionand find the expression of the expected response time for the TLPS model. TLPSscheduling discipline can be applied to size-based differentiation in TCP/IPnetworks and Web server request handling.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Unconstrained CO2 emission from fossil fuel burning has been the dominantcause of observed anthropogenic global warming. The amounts of \"proven\" andpotential fossil fuel reserves are uncertain and debated. Regardless of thetrue values, society has flexibility in the degree to which it chooses toexploit these reserves, especially unconventional fossil fuels and thoselocated in extreme or pristine environments. If conventional oil productionpeaks within the next few decades, it may have a large effect on futureatmospheric CO2 and climate change, depending upon subsequent energy choices.Assuming that proven oil and gas reserves do not greatly exceed estimates ofthe Energy Information Administration, and recent trends are toward lowerestimates, we show that it is feasible to keep atmospheric CO2 from exceedingabout 450 ppm by 2100, provided that emissions from coal, unconventional fossilfuels, and land use are constrained. Coal-fired power plants withoutsequestration must be phased out before mid-century to achieve this CO2 limit.It is also important to \"stretch\" conventional oil reserves via energyconservation and efficiency, thus averting strong pressures to extract liquidfuels from coal or unconventional fossil fuels while clean technologies arebeing developed for the era \"beyond fossil fuels\". We argue that a rising priceon carbon emissions is needed to discourage conversion of the vast fossilresources into usable reserves, and to keep CO2 beneath the 450 ppm ceiling.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present follow-up observations of pulsating subdwarf B (sdB) stars as partof our efforts to resolve the pulsation spectra for use in asteroseismologicalanalyses. This paper reports on multisite campaigns of the pulsating sdB starsPG 1618+563B and PG 0048+091. Data were obtained from observatories placedaround the globe for coverage from all longitudes. For PG 1618+563B, ourfive-site campaign uncovered a dichotomy of pulsation states: Early during thecampaign the amplitudes and phases (and perhaps frequencies) were quitevariable while data obtained late in the campaign were able to fully resolvefive stable pulsation frequencies. For PG 0048+091, our five-site campaignuncovered a plethora of frequencies with short pulsation lifetimes. We findthem to have observed properties consistent with stochastically excitedoscillations, an unexpected result for subdwarf B stars. We discuss ourfindings and their impact on subdwarf B asteroseismology.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We consider single-file diffusion in an open system with two species $A,B$ ofparticles. At the boundaries we assume different reservoir densities whichdrive the system into a non-equilibrium steady state. As a model we use anone-dimensional two-component simple symmetric exclusion process with twodifferent hopping rates $D_A,D_B$ and open boundaries. For investigating thedynamics in the hydrodynamic limit we derive a system of coupled non-lineardiffusion equations for the coarse-grained particle densities. The relaxationof the initial density profile is analyzed by numerical integration. Exactanalytical expressions are obtained for the self-diffusion coefficients, whichturns out to be length-dependent, and for the stationary solution. In thesteady state we find a discontinuous boundary-induced phase transition as thetotal exterior density gradient between the system boundaries is varied. At oneboundary a boundary layer develops inside which the current flows against thelocal density gradient. Generically the width of the boundary layer and thebulk density profiles do not depend on the two hopping rates. At the phasetransition line, however, the individual density profiles depend strongly onthe ratio $D_A/D_B$. Dynamic Monte Carlo simulation confirm our theoreticalpredictions.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Extending network lifetime of battery-operated devices is a key design issuethat allows uninterrupted information exchange among distributive nodes inwireless sensor networks. Collaborative beamforming (CB) and cooperativetransmission (CT) have recently emerged as new communication techniques thatenable and leverage effective resource sharing among collaborative/cooperativenodes. In this paper, we seek to maximize the lifetime of sensor networks byusing the new idea that closely located nodes can use CB/CT to reduce the loador even avoid packet forwarding requests to nodes that have critical batterylife. First, we study the effectiveness of CB/CT to improve the signal strengthat a faraway destination using energy in nearby nodes. Then, a 2D disk case isanalyzed to assess the resulting performance improvement. For general networks,if information-generation rates are fixed, the new routing problem isformulated as a linear programming problem; otherwise, the cost for routing isdynamically adjusted according to the amount of energy remaining and theeffectiveness of CB/CT. From the analysis and simulation results, it is seenthat the proposed schemes can improve the lifetime by about 90% in the 2D disknetwork and by about 10% in the general networks, compared to existing schemes.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We propose a scheme for generating squeezed states in solid state circuitsconsisting of a nanomechanical resonator (NMR), a superconducting Cooper-pairbox (CPB) and a superconducting transmission line resonator (STLR). Thenonlinear interaction between the NMR and the STLR can be implemented bysetting the external biased flux of the CPB at certain values. The interactionHamiltonian between the NMR and the STLR is derived by performing Fr$\\rm\\ddoto$hlich transformation on the total Hamiltonian of the combined system. Just byadiabatically keeping the CPB at the ground state, we get the standardparametric down-conversion Hamiltonian. The CPB plays the role of ``nonlinearmedia\", and the squeezed states of the NMR can be easily generated in a mannersimilar to the three-wave mixing in quantum optics. This is the three-wavemixing in a solid-state circuit.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Long-lived, heavy particles are predicted in a number of models beyond thestandard model of particle physics. We present the first direct search for suchparticles' decays, occurring up to 100 hours after their production and notsynchronized with an accelerator bunch crossing. We apply the analysis to thegluino (~g), predicted in split supersymmetry, which after hadronization canbecome charged and lose enough momentum through ionization to come to rest indense particle detectors. Approximately 410 pb^-1 of p-pbar collisions at 1.96TeV collected with the D0 detector during Run II of the Fermilab Tevatroncollider are analyzed in search of such ``stopped gluinos'' decaying into agluon and a neutralino (~X_0), reconstructed as a jet and missing energy. Noexcess is observed above background, and limits are placed on the (gluino crosssection) x (probability to stop) x BR(~g -> g ~X_0) as a function of the gluinoand ~X_0 masses, for gluino lifetimes from 30 $\\mu$s -- 100 hours.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "In this work we compare numerically exact Quantum Monte Carlo (QMC)calculations and Green function theory (GFT) calculations of thin ferromagneticfilms including second order anisotropies. Thereby we concentrate on easy planesystems, i.e. systems for which the anisotropy favors a magnetization parallelto the film plane. We discuss these systems in perpendicular external field,i.e. B parallel to the film normal. GFT results are in good agreement with QMCfor high enough fields and temperatures. Below a critical field or a criticaltemperature no collinear stable magnetization exists in GFT. On the other handQMC gives finite magnetization even below those critical values. This indicatesthat there occurs a transition from non-collinear to collinear configurationswith increasing field or temperature. For slightly tilted external fields arotation of magnetization from out-of-plane to in-plane orientation is foundwith decreasing temperature.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The gravitational field of both local and global non static cosmic strings inthe context of Lyra geometry are investigated. Local strings are characterizedby having an energy momentum tensor whose only non null components are $T_{tt}= T_{zz}$ . As linearized Einstein equations are formally analogous to theMaxwell equations, the exterior solution does not depend on the radialdistribution of the source and hence a Dirac d function was used to approximatethe radial distribution of the energy momentum tensor for a local cosmic stringalong the z-axis: $T_{ab} = \\delta(x) \\delta(y)diag (\\sigma, 0, 0, \\sigma) $,$\\sigma $being the energy density of the string [A.Vilenkin.Phys.Rep.(1985)121,263]. For a global string, the energy momentum tensorcomponents are calculated from the action density for a complex scalar field yalong with a Maxican hat potential. The gravitational field of the globalstring is shown to be attractive in nature.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "In this paper we outline some aspects of nonabelian gauged linear sigmamodels. First, we review how partial flag manifolds (generalizingGrassmannians) are described physically by nonabelian gauged linear sigmamodels, paying attention to realizations of tangent bundles and other aspectspertinent to (0,2) models. Second, we review constructions of Calabi-Yaucomplete intersections within such flag manifolds, and properties of the gaugedlinear sigma models. We discuss a number of examples of nonabelian GLSM's inwhich the Kahler phases are not birational, and in which at least one phase isrealized in some fashion other than as a complete intersection, extendingprevious work of Hori-Tong. We also review an example of an abelian GLSMexhibiting the same phenomenon. We tentatively identify the mathematicalrelationship between such non-birational phases, as examples of Kuznetsov'shomological projective duality. Finally, we discuss linear sigma model modulispaces in these gauged linear sigma models. We argue that the moduli spacesbeing realized physically by these GLSM's are precisely Quot and hyperquotschemes, as one would expect mathematically.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We investigate the possibility of discriminating between Modified NewtonianDynamics (MOND) and Newtonian gravity with dark matter, by studying thevertical dynamics of disk galaxies. We consider models with the same circularvelocity in the equatorial plane (purely baryonic disks in MOND and the samedisks in Newtonian gravity embedded in spherical dark matter haloes), and weconstruct their intrinsic and projected kinematical fields by solving the Jeansequations under the assumption of a two-integral distribution function. Wefound that the vertical velocity dispersion of deep-MOND disks can be muchlarger than in the equivalent spherical Newtonian models. However, in the morerealistic case of high-surface density disks this effect is significantlyreduced, casting doubts on the possibility of discriminating between MOND andNewtonian gravity with dark matter by using current observations.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Direct photons provide a insightful tool to study the different stages of aheavy ion collision, especially the formation of a quark-gluon plasma, withoutbeing influenced by the strong interaction and hadronization processes. Theyield of direct photons can be determined based on the inclusive photon yieldand the background from hadronic decays. We present a new analysis techniqueapplied to PHENIX Run4 Au+Au dataset. It uses strict particleidentification(PID) in the Electromagnetic Calorimeter(EMCal) and a chargedparticle veto to extract a clean photon signal. These photons are then taggedwith EMCal photon candidates with loose PID cuts, which can be reconstructedwith high efficiency, to determine the fraction of photons originating from$\\pi^{0}$ decays. Many systematic uncertainties and detector effects cancel inthis method.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Reflectance, transmittance and absorbance of a symmetric light pulse, thecarrying frequency of which is close to the frequency of interband transitionsin a quantum well, are calculated. Energy levels of the quantum well areassumed discrete, and two closely located excited levels are taken intoaccount. A wide quantum well (the width of which is comparable to the length ofthe light wave, corresponding to the pulse carrying frequency) is considered,and the dependance of the interband matrix element of the momentum operator onthe light wave vector is taken into account. Refractive indices of barriers andquantum well are assumed equal each other. The problem is solved for anarbitrary ratio of radiative and nonradiative lifetimes of electronicexcitations. It is shown that the spatial dispersion essentially affects theshapes of reflected and transmitted pulses. The largest changes occur when theradiative broadening is close to the difference of frequencies of interbandtransitions taken into account.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We study electrical excitation of nonlinear plasma waves in heterostructureswith two-dimensional electron channels and with split gates, and thepropagation of these waves using hydrodynamic equations for electron transportcoupled with two-dimensional Poisson equation for self-consistent electricpotential. The term related to electron collisions with impurities and phononsas well as the term associated with viscosity are included into thehydrodynamic equations. We demonstrate the formation of shock and soliton-likewaves as a result of the evolution of strongly nonuniform initial electrondensity distribution. It is shown that the shock wave front and the shape ofsoliton-like pulses pronouncedly depend on the coefficient of viscosity, thethickness of the gate layer and the nonuniformity of the donor distributionalong the channel. The electron collisions result in damping of the shock andsoliton-like waves, while they do not markedly affect the thickness of theshock wave front.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We have used Suprime-Cam on the Subaru Telescope to conduct a V- and I-bandimaging survey of fields sampling the spheroid of the Andromeda galaxy alongits south-east minor axis. Our photometric data are deep enough to resolvestars down to the red clump. Based on a large and reliable sample of red giantstars available from this deep wide-field imager, we have derived metallicitydistributions vs. radius and a surface brightness profile over projecteddistances of R=23-66 kpc from the galaxy's center. The metallicitydistributions across this region shows a clear high mean metallicity and abroad distribution ([Fe/H] ~ -0.6 +/- 0.5), and indicates no metallicitygradient within our observed range. The surface brightness profile at R>40 kpcis found to be flatter than previously thought. It is conceivable that thispart of the halo samples as yet unidentified, metal-rich substructure.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The paper is devoted to classification problem of finite dimensional complexnone Lie filiform Leibniz algebras. Actually, the observations show there aretwo resources to get classification of filiform Leibniz algebras. The first ofthem is naturally graded none Lie filiform Leibniz algebras and the another oneis naturally graded filiform Lie algebras. Using the first resource we get twodisjoint classes of filiform Leibniz algebras. The present paper deals with thesecond of the above two classes, the first class has been considered in ourprevious paper. The algebraic classification here means to specify therepresentatives of the orbits, whereas the geometric classification is theproblem of finding generic structural constants in the sense of algebraicgeometry. Our main effort in this paper is the algebraic classification. Wesuggest here an algebraic method based on invariants. Utilizing this method forany given low dimensional case all filiform Leibniz algebras can be classified.Moreover, the results can be used for geometric classification of orbits ofsuch algebras.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "A general and basic model of primordial evolution--a soup of reactingfinitary and discrete processes--is employed to identify and analyzefundamental mechanisms that generate and maintain complex structures inprebiotic systems. The processes--$\\epsilon$-machines as defined incomputational mechanics--and their interaction networks both provide welldefined notions of structure. This enables us to quantitatively demonstratehierarchical self-organization in the soup in terms of complexity. We foundthat replicating processes evolve the strategy of successively building higherlevels of organization by autocatalysis. Moreover, this is facilitated by localcomponents that have low structural complexity, but high generality. In effect,the finitary process soup spontaneously evolves a selection pressure thatfavors such components. In light of the finitary process soup's generality,these results suggest a fundamental law of hierarchical systems: globalcomplexity requires local simplicity.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We report the recent results of the magnetic transitions and axial-vectortransitions of the baryon antidecuplet within the framework of the chiralquark-soliton model. The dynamical model parameters are fixed by experimentaldata for the magnetic moments of the baryon octet, for the hyperon semileptonicdecay constants, and for the singlet axial-vector constant. The transitionmagnetic moments $\\mu_{\\Lambda\\Sigma}$ and $\\mu_{N\\Delta}$ are well reproducedand other octet-decuplet and octet-antidecuplet transitions are predicted. Inparticular, the present calculation of $\\mu_{\\Sigma\\Sigma^*}$ is found to bebelow the upper bound $0.82\\mu_N$ that the SELEX collaboration measured veryrecently. The results explains consistently the recent findings of a new $N^*$resonance from the GRAAL and Tohoku LNS group. We also obtain the transitionaxial-vector constants for the $\\Theta^+\\to KN$ from which the decay width ofthe $\\Theta^{+}$ pentaquark baryon is determined as a function of thepion-nucleon sigma term $\\Sigma_{\\pi N}$. We investigate the dependence of thedecay width of the $\\Theta^{+}$ on the $g_{A}^{(0)}$, with the $g_{A}^{(0)}$varied within the range of the experimental uncertainty. We show that a smalldecay width of the $\\Theta^{+}\\to KN$, i.e. $\\Gamma_{\\Theta KN} \\leq 1$ MeV, iscompatible with the values of all known semileptonic decays with the generallyaccepted value of $g_{A}^{(0)} \\approx 0.3$ for the proton.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The bright X-ray transient H 1743-322 was observed daily by the Rossi X-rayTiming Explorer (RXTE) during most of its 8-month outburst in 2003. We presenta detailed spectral analysis and a supporting timing analysis of all of thesedata, and we discuss the behavior and evolution of the source in terms of thethree principal X-ray states defined by Remillard and McClintock. These X-rayresults are complemented by Very Large Array (VLA) data obtained at sixfrequencies that provide quite complete coverage of the entire outburst cycleat 4.860 GHz and 8.460 GHz. We also present photometric data and finding chartsfor the optical counterpart in both outburst and quiescence. We closely compareH 1743-322 to the well-studied black-hole X-ray transient XTE J1550-564 andfind the behaviors of these systems to be very similar. As reported elsewhere,both H 1743-322 and XTE J1550-564 are relativistic jet sources and both exhibita pair of high-frequency QPO oscillations with a 3:2 frequency ratio. The manystriking similarities between these two sources argue strongly that H 1743-322is a black hole binary, although presently no dynamical data exist to supportthis conclusion.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Let $\\Dh$ and $A$ be unital and separable $C^{*}$-algebras; let $\\Dh$ bestrongly self-absorbing. It is known that any two unital $^*$-homomorphismsfrom $\\Dh$ to $A \\otimes \\Dh$ are approximately unitarily equivalent. We showthat, if $\\Dh$ is also $K_{1}$-injective, they are even asymptoticallyunitarily equivalent. This in particular implies that any unital endomorphismof $\\Dh$ is asymptotically inner. Moreover, the space of automorphisms of $\\Dh$is compactly-contractible (in the point-norm topology) in the sense that forany compact Hausdorff space $X$, the set of homotopy classes $[X,\\Aut(\\Dh)]$reduces to a point. The respective statement holds for the space of unitalendomorphisms of $\\Dh$. As an application, we give a description of theKasparov group $KK(\\Dh, A\\ot \\Dh)$ in terms of $^*$-homomorphisms andasymptotic unitary equivalence. Along the way, we show that the Kasparov group$KK(\\Dh, A\\ot \\Dh)$ is isomorphic to $K_0(A\\ot \\Dh)$.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We investigate the mixing-demixing transition and the collapse in aquasi-two-dimensional degenerate boson-fermion mixture (DBFM) with a bosonicvortex. We solve numerically a quantum-hydrodynamic model based on a newdensity functional which accurately takes into account the dimensionalcrossover. It is demonstrated that with the increase of interspecies repulsion,a mixed state of DBFM could turn into a demixed state. The system collapses forinterspecies attraction above a critical value which depends on the vortexquantum number. For interspecies attraction just below this critical limitthere is almost complete mixing of boson and fermion components. Such mixed anddemixed states of a DBFM could be experimentally realized by varying anexternal magnetic field near a boson-fermion Feshbach resonance, which willresult in a continuous variation of interspecies interaction.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The distributed source coding problem is considered when the sensors, orencoders, are under Byzantine attack; that is, an unknown number of sensorshave been reprogrammed by a malicious intruder to undermine the reconstructionat the fusion center. Three different forms of the problem are considered. Thefirst is a variable-rate setup, in which the decoder adaptively chooses therates at which the sensors transmit. An explicit characterization of thevariable-rate minimum achievable sum rate is stated, given by the maximumentropy over the set of distributions indistinguishable from the true sourcedistribution by the decoder. In addition, two forms of the fixed-rate problemare considered, one with deterministic coding and one with randomized coding.The achievable rate regions are given for both these problems, with a largerregion achievable using randomized coding, though both are suboptimal comparedto variable-rate coding.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Given an isometric immersion $f\\colon M^n\\to \\R^{n+1}$ of a compactRiemannian manifold of dimension $n\\geq 3$ into Euclidean space of dimension$n+1$, we prove that the identity component $Iso^0(M^n)$ of the isometry group$Iso(M^n)$ of $M^n$ admits an orthogonal representation $\\Phi\\colonIso^0(M^n)\\to SO(n+1)$ such that $f\\circ g=\\Phi(g)\\circ f$ for every $g\\inIso^0(M^n)$. If $G$ is a closed connected subgroup of $Iso(M^n)$ acting locallypolarly on $M^n$, we prove that $\\Phi(G)$ acts polarly on $\\R^{n+1}$, and weobtain that $f(M^n)$ is given as $\\Phi(G)(L)$, where $L$ is a hypersurface of asection which is invariant under the Weyl group of the $\\Phi(G)$-action. Wealso find several sufficient conditions for such an $f$ to be a rotationhypersurface. Finally, we show that compact Euclidean rotation hypersurfaces ofdimension $n\\geq 3$ are characterized by their underlying warped productstructure.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present a measurement of the top-quark mass in $p\\bar p$ collisions at\\hbox{$\\sqrt{s}=1.96$} TeV which uses events with an inclusive signature ofmissing transverse energy and jets. % The event selection is sensitive to$t\\bar t\\to W^+bW^-\\bar b\\to l\\nu b q q^\\prime \\bar b$ independent of thelepton flavor, and results in a large acceptance for $W\\to\\tau\\nu$ decays. %All-hadronic $t\\bar t$ decays and events with identified electrons or muons arevetoed to provide a statistically independent sample with respect to allprevious measurements. % The top-quark mass is inferred from the distributionof the scalar sum of all jet transverse energies and the missing transverseenergy. Using 311 pb$^{-1}$ of integrated luminosity recorded by the ColliderDetector at Fermilab, we measure a top-quark mass $m_t = 172.3^{+10.8}_{-9.6}$(stat.)$\\pm 10.8$(syst.) GeV/$c^2$. While the uncertainty on$m_t$ is larger than that of other measurements, the result is statisticallyuncorrelated with those of other methods, and thus can help to reduce theoverall $m_t$ uncertainty when combined with other existing measurements.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "A fundamental problem in neuroscience is understanding how working memory --the ability to store information at intermediate timescales, like 10s ofseconds -- is implemented in realistic neuronal networks. The most likelycandidate mechanism is the attractor network, and a great deal of effort hasgone toward investigating it theoretically. Yet, despite almost a quartercentury of intense work, attractor networks are not fully understood. Inparticular, there are still two unanswered questions. First, how is it thatattractor networks exhibit irregular firing, as is observed experimentallyduring working memory tasks? And second, how many memories can be stored underbiologically realistic conditions? Here we answer both questions by studying anattractor neural network in which inhibition and excitation balance each other.Using mean field analysis, we derive a three-variable description of attractornetworks. From this description it follows that irregular firing can exist onlyif the number of neurons involved in a memory is large. The same mean fieldanalysis also shows that the number of memories that can be stored in a networkscales with the number of excitatory connections, a result that has beensuggested for simple models but never shown for realistic ones. Both of thesepredictions are verified using simulations with large networks of spikingneurons.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Despite their claimed biological plausibility, most self organizing networkshave strict topological constraints and consequently they cannot take intoaccount a wide range of external stimuli. Furthermore their evolution isconditioned by deterministic laws which often are not correlated with thestructural parameters and the global status of the network, as it should happenin a real biological system. In nature the environmental inputs are noiseaffected and fuzzy. Which thing sets the problem to investigate the possibilityof emergent behaviour in a not strictly constrained net and subjected todifferent inputs. It is here presented a new model of Evolutionary Neural Gas(ENG) with any topological constraints, trained by probabilistic laws dependingon the local distortion errors and the network dimension. The network isconsidered as a population of nodes that coexist in an ecosystem sharing localand global resources. Those particular features allow the network to quicklyadapt to the environment, according to its dimensions. The ENG model analysisshows that the net evolves as a scale-free graph, and justifies in a deeplyphysical sense- the term gas here used.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Recent studies of the near-infrared (NIR) properties of dwarf irregulargalaxies (dIs) and blue compact dwarfs (BCDs) have provided improved estimatesfor the NIR luminosity of old stellar populations in these galaxies. These canbe used to derive gas fractions, and thereby to evaluate how BCDs have evolvedwith respect to dIs. Oxygen abundances have been derived for four BCDs in theVirgo Cluster from a run at Gemini-North in 2003. Combining these newabundances with published values, we study the correlations among themetallicity, Ks luminosity, gas mass, baryonic mass, and gas fraction. Withinerrors, the two types of dwarfs appear to share a common relation between theoxygen abundance and the luminosity in Ks. The correlation between metallicityand the gas fraction is the same for BCDs as for dIs, indicating that BCDevolution has been similar to dIs. Since dIs appear to have evolved as isolatedsystems, the BCD bursts are unlikely to be a consequence of gas infall ormerging.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The identification of basaltic asteroids in the asteroid Main Belt and thedescription of their surface mineralogy is necessary to understand thediversity in the collection of basaltic meteorites. Basaltic asteroids can beidentified from their visible reflectance spectra and are classified as V-typein the usual taxonomies. In this work, we report visible spectroscopicobservations of two candidate V-type asteroids, (7472) Kumakiri and (10537)1991 RY16, located in the outer Main Belt (a > 2.85 UA). These candidate havebeen previously identified by Roig and Gil-Hutton (2006, Icarus 183, 411) usingthe Sloan Digital Sky Survey colors. The spectroscopic observations have beenobtained at the Calar Alto Observatory, Spain, during observational runs inNovember and December 2006. The spectra of these two asteroids show the steepslope shortwards of 0.70 microns and the deep absorption feature longwards of0.75 microns that are characteristic of V-type asteroids. However, the presenceof a shallow but conspicuous absorption band around 0.65 microns opens somequestions about the actual mineralogy of these two asteroids. Such band hasnever been observed before in basaltic asteroids with the intensity we detectedit. We discuss the possibility for this shallow absorption feature to be causedby the presence of chromium on the asteroid surface. Our results indicate that,together with (1459) Magnya, asteroids (7472) Kumakiri and (10537) 1991 RY16may be the only traces of basaltic material found up to now in the outer MainBelt.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The absolute calibration and characterization of the Multiband ImagingPhotometer for Spitzer (MIPS) 70 micron coarse- and fine-scale imaging modesare presented based on over 2.5 years of observations. Accurate photometry(especially for faint sources) requires two simple processing steps beyond thestandard data reduction to remove long-term detector transients. Point spreadfunction (PSF) fitting photometry is found to give more accurate flux densitiesthan aperture photometry. Based on the PSF fitting photometry, the calibrationfactor shows no strong trend with flux density, background, spectral type,exposure time, or time since anneals. The coarse-scale calibration sampleincludes observations of stars with flux densities from 22 mJy to 17 Jy, onbackgrounds from 4 to 26 MJy sr^-1, and with spectral types from B to M. Thecoarse-scale calibration is 702 +/- 35 MJy sr^-1 MIPS70^-1 (5% uncertainty) andis based on measurements of 66 stars. The instrumental units of the MIPS 70micron coarse- and fine-scale imaging modes are called MIPS70 and MIPS70F,respectively. The photometric repeatability is calculated to be 4.5% from twostars measured during every MIPS campaign and includes variations on all timescales probed. The preliminary fine-scale calibration factor is 2894 +/- 294MJy sr^-1 MIPS70F^-1 (10% uncertainty) based on 10 stars. The uncertainty inthe coarse- and fine-scale calibration factors are dominated by the 4.5%photometric repeatability and the small sample size, respectively. The 5-sigma,500 s sensitivity of the coarse-scale observations is 6-8 mJy. This work showsthat the MIPS 70 micron array produces accurate, well calibrated photometry andvalidates the MIPS 70 micron operating strategy, especially the use of frequentstimulator flashes to track the changing responsivities of the Ge:Ga detectors.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We detected X-ray emission from the 50-kyr-old pulsar J1809-1917 and resolvedits pulsar wind nebula (PWN) with Chandra. The pulsar spectrum fits PL+BB modelwith the photon index of 1.2 and the BB temperature of 2 MK for n_{H}=0.7\\times10^{22} cm^{-2}. The luminosities are(4\\pm 1)\\times 10^{31} ergs s^{-1} for thePL component (in the 0.5-8 keV band) and ~1\\times 10^{32} ergs s^{-1} for theBB component (bolometric) at a plausible distance of 3.5 kpc. The bright innerPWN component of a 3''\\times12'' size is elongated in the north-southdirection, with the pulsar close to its south end. This component is immersedin a larger (20''\\times40''), similarly elongated outer PWN component of lowersurface brightness. The elongated shape of the compact PWN can be explained bythe ram pressure confinement of the pulsar wind due to the supersonic motion ofthe pulsar. The PWN spectrum fits a PL model with photon index of 1.4\\pm0.1 and0.5-8 keV luminosity of 4\\times10^{32} ergs s^{-1}. The compact PWN appears tobe inside a large-scale (~4'\\times4') emission more extended to the south ofthe pulsar, i.e. in the direction of the alleged pulsar motion. To explain theextended X-ray emission ahead of the moving pulsar, one has to invoke strongintrinsic anisotropy of the pulsar wind or assume that this emission comes froma relic PWN swept by the asymmetrical reverse SNR shock. The pulsar and its PWNare located within the extent of the unidentified TeV source HESS J1809-193whose brightest part is offset by ~8' to the south of the pulsar, i.e. in thesame direction as the large-scale X-ray emission. Although the associationbetween J1809-1917 and HESS J1809-193 is plausible, an alternative source ofrelativistic electrons powering HESS J1809-193 might be the serendipitouslydiscovered X-ray source CXOU J180940.7-192544.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The upper critical field $H_{c2}$ is one of the many non conventionalproperties of high-$T_c$ cuprates. It is possible that the $H_{c2}(T)$anomalies are due to the presence of inhomogeneities in the local chargecarrier density $\\rho$ of the $CuO_2$ planes. In order to study this point, wehave prepared good quality samples of polycrystalline $La_{2-x}Sr_xCuO_{4}$using the wet-chemical method, which has demonstrated to produce samples with abetter cation distribution. In particular, we have studied the temperaturedependence of the second critical field, $H_{c2}(T)$, through the magnetizationmeasurements on two samples with opposite average carrier concentration($\\rho_m=x$) and nearly the same critical temperature, namely $\\rho_m = 0.08$(underdoped) and $\\rho_m = 0.25$ (overdoped). The results close to $T_c$ do notfollow the usual Ginzburg-Landau theory and are interpreted by a theory whichtakes into account the influence of the inhomogeneities.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We study universal compression of sequences generated by monotonicdistributions. We show that for a monotonic distribution over an alphabet ofsize $k$, each probability parameter costs essentially $0.5 \\log (n/k^3)$ bits,where $n$ is the coded sequence length, as long as $k = o(n^{1/3})$. Otherwise,for $k = O(n)$, the total average sequence redundancy is $O(n^{1/3+\\epsilon})$bits overall. We then show that there exists a sub-class of monotonicdistributions over infinite alphabets for which redundancy of$O(n^{1/3+\\epsilon})$ bits overall is still achievable. This class containsfast decaying distributions, including many distributions over the integers andgeometric distributions. For some slower decays, including other distributionsover the integers, redundancy of $o(n)$ bits overall is achievable, where amethod to compute specific redundancy rates for such distributions is derived.The results are specifically true for finite entropy monotonic distributions.Finally, we study individual sequence redundancy behavior assuming a sequenceis governed by a monotonic distribution. We show that for sequences whoseempirical distributions are monotonic, individual redundancy bounds similar tothose in the average case can be obtained. However, even if the monotonicity inthe empirical distribution is violated, diminishing per symbol individualsequence redundancies with respect to the monotonic maximum likelihooddescription length may still be achievable.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "It is presumed that the observed cosmic rays up to about $3\\times 10^{18}$ eVare of Galactic origin, the particles being the ones which are found in thecomposition of the stellar winds of stars that explode as supernova into theinterstellar medium (ISM) or into their winds. These particles are acceleratedin the supernova shock. In order to obtain the observed cosmic ray spectrum itis necessary to take into account the diffusive losses in the Galaxy (which aremaking the energy spectrum more steeper). Another modification of the sourcespectrum is due to the fragmentation (spallation) of the cosmic ray particles,after their collision with the ISM atoms. In this paper we are proving thatsome particles are injected in the supernova shock one or two time ionized,and, also, that the contribution of massive stars ($30 M_{\\odot}\\leq M\\leq 50M_{\\odot}$) accelerated particles to cosmic rays (where the winds are highlyenriched in heavy elements) is 1:2 for elements with $Z\\geq 6$. Another goal ofthis paper is to check if the particles are injected with the same velocity,energy or momentum.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The formation of the circumbinary envelope of Cygnus X-3 was studied byparticle simulations of the WR (Wolf Rayet) companion wind. Light curvesresulting from electron scattering absorption in this envelope were computedand compared with observed IBIS/ISGRI and BATSE light curves. The matching wasrelatively good. For reasonable values of binary parameters (masses,inclination) and wind velocities, a stable envelope was formed during a fewbinary orbits. Assuming approximately 10^-6 solar mass/year for the rate of theWR-wind, the observed light curves and accretion luminosity can be re-produced(assuming Thomson scattering opacity in the ionized He-rich envelope). Theilluminated envelope can also model the CHANDRA-spectrum using thephotoionizing XSTAR-code. Furthermore, we discuss observed radial velocitycurves of IR emission lines in the context of simulated velocity fields andfind good agreement.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "To provide criteria in the selection of target events preferable forplanetary lensing follow-up observations, we investigate the variation of theprobability of detecting planetary signals depending on the observables of thelensing magnification and source brightness. In estimating the probability, weconsider variation of the photometric precision by using a quantity defined asthe ratio of the fractional deviation of the planetary perturbation to thephotometric precision. From this investigation, we find consistent result fromprevious studies that the probability increases with the increase of themagnification. The increase rate is boosted at a certain magnification at whichperturbations caused by central caustic begin to occur. We find this boostoccurs at moderate magnifications of $A\\lesssim 20$, implying that probabilitycan be high even for events with moderate magnifications. The probabilityincreases as the source brightness increases. We find that the probability ofevents associated with stars brighter than clump giants is not negligible evenat magnifications as low as $A\\sim 5$. In the absence of rare the prime targetof very high-magnification events, we, therefore, recommend to observe eventswith brightest source stars and highest magnifications among the alertedevents. Due to the increase of the source size with the increase of thebrightness, however, the probability rapidly drops off beyond a certainmagnification, causing detections of low mass ratio planets ($q\\lesssim10^{-4}$) difficult from the observations of events involved with giant starswith magnifications $A\\gtrsim 70$.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "In this paper, we model the evolution and self-assembly of randomly orientedcarbon nanotubes (CNTs), grown on a metallic substrate in the form of a thinfilm for field emission under diode configuration. Despite high output, thecurrent in such a thin film device often decays drastically. The present paperis focused on understanding this problem. A systematic, multiphysics basedmodelling approach is proposed. First, a nucleation coupled model fordegradation of the CNT thin film is derived, where the CNTs are assumed todecay by fragmentation and formation of clusters. The random orientation of theCNTs and the electromechanical interaction are then modeled to explain theself-assembly. The degraded state of the CNTs and the electromechanical forceare employed to update the orientation of the CNTs. Field emission current atthe device scale is finally obtained by using the Fowler-Nordheim equation andintegration over the computational cell surfaces on the anode side. Thesimulated results are in close agreement with the experimental results. Basedon the developed model, numerical simulations aimed at understanding theeffects of various geometric parameters and their statistical features on thedevice current history are reported.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "A time series delta(n), the fluctuation of the nth unfolded eigenvalue wasrecently characterized for the classical Gaussian ensembles of NxN randommatrices (GOE, GUE, GSE). It is investigated here for the beta-Hermite ensembleas a function of beta (zero or positive) by Monte Carlo simulations. Thefluctuation of delta(n) and the autocorrelation function vary logarithmicallywith n for any beta>0 (1<<n<<N). The simple logarithmic behavior reported forthe higher-order moments of delta(n) for the GOE (beta=1) and the GUE (beta=2)is valid for any positive beta and is accounted for by Gaussian distributionswhose variances depend linearly on ln(n). The 1/f noise previously demonstratedfor delta(n) series of the three Gaussian ensembles, is characterized bywavelet analysis both as a function of beta and of N. When beta decreases from1 to 0, for a given and large enough N, the evolution from a 1/f noise atbeta=1 to a 1/f^2 noise at beta=0 is heterogeneous with a ~1/f^2 noise at thefinest scales and a ~1/f noise at the coarsest ones. The range of scales inwhich a ~1/f^2 noise predominates grows progressively when beta decreases.Asymptotically, a 1/f^2 noise is found for beta=0 while a 1/f noise is the rulefor beta positive.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The global colors of galaxies have recently been shown to follow bimodaldistributions. Galaxies separate into a ``red sequence'', populatedprototypically by early-type galaxies, and a ``blue cloud'', whose typicalobjects are late-type disk galaxies. Intermediate-type (Sa-Sbc) galaxiespopulate both regions. It has been suggested that this bimodality reflects thetwo-component nature of disk-bulge galaxies. However, it has now beenestablished that there are two types of bulges: ``classical bulges'' that aredynamically hot systems resembling (little) ellipticals, and ``pseudobulges'',dynamically cold, flattened, disk-like structures that could not have formedvia violent relaxation. Therefore thee question is whether at types Sa-Sbc,where both bulge types are found, the red-blue dichotomy separates galaxies atsome value of disk-to-bulge ratio, $B/T$, or, whether it separates galaxies ofdifferent bulge type, irrespective of their $B/T$. We identify classical bulgesand pseudobulges morphologically with HST images in a sample of nearbygalaxies. Detailed surface photometry reveals that: (1) The red -- bluedichotomy is a function of bulge type: at the same $B/T$, pseudobulges are inglobally blue galaxies and classical bulges are in globally red galaxies. (2)Bulge type also predicts where the galaxy lies in other (bimodal) globalstructural parameters. (3) Hence, the red -- blue dichotomy is not due todecreasing bulge prominence alone, and the bulge type of a galaxy carriessignificance for the galaxy's evolutionary history ... (Abridged)", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We explore the morphology of hard (18-30 keV) X-ray emission from the Comacluster of galaxies. We analyze a deep (1.1 Ms) observation of the Coma clusterwith the ISGRI imager on board the \\emph{INTEGRAL} satellite. We show that thesource extension in the North-East to South-West (SW) direction ($\\sim 17'$)significantly exceeds the size of the point spread function of ISGRI, and thatthe centroid of the image of the source in the 18-30 keV band is displaced inthe SW direction compared to the centroid in the 1-10 keV band. To test thenature of the SW extension we fit the data assuming different models of sourcemorphology. The best fit is achieved with a diffuse source of elliptical shape,although an acceptable fit can be achieved assuming an additional point sourceSW of the cluster core. In the case of an elliptical source, the direction ofextension of the source coincides with the direction toward the subclusterfalling onto the Coma cluster. If the SW excess is due to the presence of apoint source with a hard spectrum, we show that there is no obvious X-raycounterpart for this additional source, and that the closest X-ray source isthe quasar EXO 1256+281, which is located $6.1'$ from the centroid of theexcess. The observed morphology of the hard X-ray emission clarifies the natureof the hard X-ray \"excess\" emission from the Coma cluster, which is due to thepresence of an extended hard X-ray source SW of the cluster core.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We establish a direct map between refined topological vertex and sl(N)homological invariants of the of Hopf link, which include Khovanov-Rozanskyhomology as a special case. This relation provides an exact answer forhomological invariants of the of Hopf link, whose components are colored byarbitrary representations of sl(N). At present, the mathematical formulation ofsuch homological invariants is available only for the fundamentalrepresentation (the Khovanov-Rozansky theory) and the relation with the refinedtopological vertex should be useful for categorifying quantum group invariantsassociated with other representations (R_1, R_2). Our result is a first directverification of a series of conjectures which identifies link homologies withthe Hilbert space of BPS states in the presence of branes, where the physicalinterpretation of gradings is in terms of charges of the branes ending onLagrangian branes.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present first results of our simulations of magnetic fields in theformation of single and binary stars using a recently developed method forincorporating Magnetohydrodynamics (MHD) into the Smoothed ParticleHydrodynamics (SPH) method. An overview of the method is presented beforediscussing the effect of magnetic fields on the formation of circumstellardiscs around young stars. We find that the presence of magnetic fields duringthe disc formation process can lead to significantly smaller and less massivediscs which are much less prone to gravitational instability. Similarly in thecase of binary star formation we find that magnetic fields, overall, suppressfragmentation. However these effects are found to be largely driven by magneticpressure. The relative importance of magnetic tension is dependent on theorientation of the field with respect to the rotation axis, but can, with theright orientation, lead to a dilution of the magnetic pressure-drivensuppression of fragmentation.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Systems of strongly correlated fermions on certain geometrically frustratedlattices at particular filling factors support excitations with fractionalcharges $\\pm e/2$. We calculate quantum mechanical ground states, low--lyingexcitations and spectral functions of finite lattices by means of numericaldiagonalization. The ground state of the most thoroughfully studied case, thecriss-crossed checkerboard lattice, is degenerate and shows long--range order.Static fractional charges are confined by a weak linear force, most probablyleading to bound states of large spatial extent. Consequently, thequasi-particle weight is reduced, which reflects the internal dynamics of thefractionally charged excitations. By using an additional parameter, wefine--tune the system to a special point at which fractional charges aremanifestly deconfined--the so--called Rokhsar--Kivelson point. For a deeperunderstanding of the low--energy physics of these models and for numericaladvantages, several conserved quantum numbers are identified.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The existence of a connected 12-regular $\\{K_4,K_{2,2,2}\\}$-ultrahomogeneousgraph $G$ is established, (i.e. each isomorphism between two copies of $K_4$ or$K_{2,2,2}$ in $G$ extends to an automorphism of $G$), with the 42 orderedlines of the Fano plane taken as vertices. This graph $G$ can be expressed in aunique way both as the edge-disjoint union of 42 induced copies of $K_4$ and asthe edge-disjoint union of 21 induced copies of $K_{2,2,2}$, with no morecopies of $K_4$ or $K_{2,2,2}$ existing in $G$. Moreover, each edge of $G$ isshared by exactly one copy of $K_4$ and one of $K_{2,2,2}$. While the linegraphs of $d$-cubes, ($3\\le d\\in\\ZZ$), are $\\{K_d, K_{2,2}\\}$-ultrahomogeneous,$G$ is not even line-graphical. In addition, the chordless 6-cycles of $G$ areseen to play an interesting role and some self-dual configurations associatedto $G$ with 2-arc-transitive, arc-transitive and semisymmetric Levi graphs areconsidered.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Thin films of Co-TiO2 are deposited on silicon and quartz substrates usingPulse Laser Deposition (PLD) process at various oxygen partial pressuresranging from 6.6 x 10-3 Pascals (Pa) to 53 Pa. Crystal structure, transport andmagnetic properties of reduced CoxTi(1-x)O2 (0 <x< 0.03) thin films areinvestigated and are found to have a strong dependence on the oxygen partialpressure. X-ray diffraction (XRD) data reveals the presence of mixed phasematerial containing both anatase and rutile. However, these phasesintertransform with the change in the oxygen partial pressure in the chamberduring the growth of the films. X-ray Photoelectron Spectroscopy (XPS) shows noCo or CoO related peaks for samples with Co concentration up to x=0.03.However, the oxygen 1s peaks are asymmetric suggesting the presence of oxygenvacancies. The transport and magnetic measurements show a clear dependence onthe concentration of oxygen vacancies. There is an enhancement in theelectrical conductivity and the magnetization as more vacancies are created inthe material. The resistivity as a function of temperature rho(T) follows thepolaronic behavior and the activation energies obtained, ~100 to 150meV, arewithin the range that is typical for semiconducting materials.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "It has recently been suggested \\cite{Chang:2006bm} that a reliable andunambiguous definition of the non-perturbative massive quark condensate couldbe provided by considering a non positive-definite class of solutions to theSchwinger Dyson Equation for the quark propagator. In this paper we show thatthis definition is incomplete without considering a third class of solutions.Indeed, studying these three classes reveals a degeneracy of possiblecondensate definitions leading to a whole range of values. However, we showthat the {\\it physical} condensate may in fact be extracted by simple fittingto the Operator Product Expansion, a procedure which is stabilised byconsidering the three classes of solution together. We find that for currentquark masses in the range from zero to 25 MeV or so (defined at a scale of 2GeV in the $\\bar{MS}$ scheme), the dynamically generated condensate increasesfrom the chiral limit in a wide range of phenomenologically successful modelsof the confining QCD interaction. Lastly, the role of a fourth class of nodedsolutions is briefly discussed.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present a formal model to represent and solve the unicast/multicastrouting problem in networks with Quality of Service (QoS) requirements. Toattain this, first we translate the network adapting it to a weighted graph(unicast) or and-or graph (multicast), where the weight on a connectorcorresponds to the multidimensional cost of sending a packet on the relatednetwork link: each component of the weights vector represents a different QoSmetric value (e.g. bandwidth, cost, delay, packet loss). The second stepconsists in writing this graph as a program in Soft Constraint LogicProgramming (SCLP): the engine of this framework is then able to find the bestpaths/trees by optimizing their costs and solving the constraints imposed onthem (e.g. delay < 40msec), thus finding a solution to QoS routing problems.Moreover, c-semiring structures are a convenient tool to model QoS metrics. Atlast, we provide an implementation of the framework over scale-free networksand we suggest how the performance can be improved.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The cycling operation is a special kind of conjugation that can be applied toelements in Artin's braid groups, in order to reduce their length. It is a keyingredient of the usual solutions to the conjugacy problem in braid groups. Intheir seminal paper on braid-cryptography, Ko, Lee et al. proposed the {\\itcycling problem} as a hard problem in braid groups that could be interestingfor cryptography. In this paper we give a polynomial solution to that problem,mainly by showing that cycling is surjective, and using a result by Maffrewhich shows that pre-images under cycling can be computed fast. This resultalso holds in every Artin-Tits group of spherical type.  On the other hand, the conjugacy search problem in braid groups is usuallysolved by computing some finite sets called (left) ultra summit sets(left-USS), using left normal forms of braids. But one can equally use rightnormal forms and compute right-USS's. Hard instances of the conjugacy searchproblem correspond to elements having big (left and right) USS's. One may thinkthat even if some element has a big left-USS, it could possibly have a smallright-USS. We show that this is not the case in the important particular caseof rigid braids. More precisely, we show that the left-USS and the right-USS ofa given rigid braid determine isomorphic graphs, with the arrows reversed, theisomorphism being defined using iterated cycling. We conjecture that the sameis true for every element, not necessarily rigid, in braid groups andArtin-Tits groups of spherical type.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Recurrent neural networks (RNNs) have proved effective at one dimensionalsequence learning tasks, such as speech and online handwriting recognition.Some of the properties that make RNNs suitable for such tasks, for examplerobustness to input warping, and the ability to access contextual information,are also desirable in multidimensional domains. However, there has so far beenno direct way of applying RNNs to data with more than one spatio-temporaldimension. This paper introduces multi-dimensional recurrent neural networks(MDRNNs), thereby extending the potential applicability of RNNs to vision,video processing, medical imaging and many other areas, while avoiding thescaling problems that have plagued other multi-dimensional models. Experimentalresults are provided for two image segmentation tasks.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "In this note, we consider possible constraints from $t \\bar t$ production onthe gauge bosons of theories with an extended strong interaction sector such asaxigluons or flavour universal colorons. Such constraints are found to becompetitive with those obtained from the dijet data. The current $t \\bar t$data from the Tevatron rule out axigluon masses ($m_A$) up to 900 GeV and 850GeV at 2 $\\sigma$ and 4 $\\sigma$ levels respectively. For the case of flavouruniversal colorons the data rule out a mass ($m_C$) below 800 GeV (780 GeV) atthe $2 (4) \\sigma $ level and also the mass range between 900 GeV to 2.1 TeV at2 $\\sigma$ level, for $\\cot \\xi = 1$, where $\\xi$ is the mixing angle. For$\\cot \\xi =2$ on the other hand, the excluded range is $m_C \\lsim 950 (920)$GeV and $m_C \\gsim 1.02 (1.15 \\lsim m_C \\lsim 1.8)$ TeV at $2 \\sigma$ ($4\\sigma $) level. We point out that for higher axigluon/coloron masses, even forthe dijet channel, the limits on the coloron mass, for $\\cot \\xi = 1$, may bedifferent than those for the axigluon. We also compute the expectedforward-backward asymmetry for the case of the axigluons which would allow itto be discriminated against the SM as also the colorons. We further find thatat the LHC, the signal should be visible in the $t \\bar t$ invariant massspectrum for a wide range of axigluon and coloron masses that are stillallowed. We point out how top polarisation may be used to further discriminatethe axigluon and coloron case from the SM as well as from each other.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The evolution of Earth-Moon system is described by the dark matter fieldfluid model proposed in the Meeting of Division of Particle and Field 2004,American Physical Society. The current behavior of the Earth-Moon system agreeswith this model very well and the general pattern of the evolution of theMoon-Earth system described by this model agrees with geological and fossilevidence. The closest distance of the Moon to Earth was about 259000 km at 4.5billion years ago, which is far beyond the Roche's limit. The result suggeststhat the tidal friction may not be the primary cause for the evolution of theEarth-Moon system. The average dark matter field fluid constant derived fromEarth-Moon system data is 4.39 x 10^(-22) s^(-1)m^(-1). This model predictsthat the Mars's rotation is also slowing with the angular acceleration rateabout -4.38 x 10^(-22) rad s^(-2).", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We study the dynamics of a single chain polymer confined to a two dimensionalcell. We introduce a kinetically constrained lattice gas model that preservesthe connectivity of the chain, and we use this kinetically constrained model tostudy the dynamics of the polymer at varying densities through Monte Carlosimulations. Even at densities close to the fully-packed configuration, we findthat the monomers comprising the chain manage to diffuse around the box with aroot mean square displacement of the order of the box dimensions over timescales for which the overall geometry of the polymer is, nevertheless, largelypreserved. To capture this shape persistence, we define the local tangent fieldand study the two-time tangent-tangent correlation function, which exhibits aglass-like behavior. In both closed and open chains, we observe reptationalmotion and reshaping through local fingering events which entail global monomerdisplacement.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "This is the second part of an article about q-deformed analogs of spinorcalculus. The considerations refer to quantum spaces of physical interest, i.e.q-deformed Euclidean space in three or four dimensions as well as q-deformedMinkowski space. The Clifford algebras corresponding to these quantum spacesare treated. Especially, their commutation relations and their Hopf structuresare written down. Bases of the four-dimensional Clifford algebras areconstructed and their properties are discussed. Matrix representations of theClifford algebras lead to q-deformed Dirac-matrices for the four-dimensionalquantum spaces. Moreover, q-analogs of the four-dimensional spin matrices arepresented. A very complete set of trace relations and rearrangement formulaeconcerning spin and Dirac-matrices is given. Dirac spinors together with theirbilinear covariants are defined. Their behavior under q-deformed Lorentztransformation is discussed in detail.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The observed correlation of oxygen vacancies and room temperatureferromagnetic ordering in Co doped ZnO1-o nanoparticles reported earlier (Naeemet al Nanotechnology 17, 2675-2680) has been further explored by transport andoptical measurements. In these particles room temperature ferromagneticordering had been observed to occur only after annealing in forming gas. In thecurrent work the optical properties have been studied by diffuse reflectionspectroscopy in the UV-Vis region and the band gap of the Co doped compositionshas been found to decrease with Co addition. Reflections minima are observed atthe energies characteristic of Co+2 d-d (tethrahedral symmetry) crystal fieldtransitions, further establishing the presence of Co in substitutional sites.Electrical transport measurements on palletized samples of the nanoparticlesshow that the effect of a forming gas is to strongly decrease the resistivitywith increasing Co concentration. For the air annealed and non-ferromagneticsamples the variation in the resistivity as a function of Co content areopposite to those observed in the particles prepared in forming gas. Theferromagnetic samples exhibit an apparent change from insulator to metal withincreasing temperatures for T>380K and this change becomes more pronounced withincreasing Co content. The magnetic and resistive behaviors are correlated byconsidering the model by Calderon et al [M. J. Calderon and S. D. Sarma, Annalsof Physics 2007 (Accepted doi: 10.1016/j.aop.2007.01.010] where theferromagnetism changes from being mediated by polarons in the low temperatureinsulating region to being mediated by the carriers released from the weaklybound states in the higher temperature metallic region.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We investigate relaxation and dephasing of an electron spin confined in asemiconductor quantum dot and subject to spin-orbit coupling. Even in vanishingmagnetic field, B = 0, slow noise coupling to the electron's orbital degree offreedom leads to dephasing of the spin due to a random, in general non-AbelianBerry phase acquired by the spin. For illustration we first present a simplequasiclassical description, then consider a model with 2 orbital states only,and finally present a perturbative quantum treatment appropriate for anelectron in a realistic (roughly parabolic, not too strongly confining) quantumdot. We further compare the effect of different sources of noise. While atlarge magnetic fields phonons dominate the relaxation processes, at low fieldselectron-hole excitations and possibly 1/f noise may dominate.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "A set of vertices $S$ \\emph{resolves} a connected graph $G$ if every vertexis uniquely determined by its vector of distances to the vertices in $S$. The\\emph{metric dimension} of $G$ is the minimum cardinality of a resolving set of$G$. Let $\\mathcal{G}_{\\beta,D}$ be the set of graphs with metric dimension$\\beta$ and diameter $D$. It is well-known that the minimum order of a graph in$\\mathcal{G}_{\\beta,D}$ is exactly $\\beta+D$. The first contribution of thispaper is to characterise the graphs in $\\mathcal{G}_{\\beta,D}$ with order$\\beta+D$ for all values of $\\beta$ and $D$. Such a characterisation waspreviously only known for $D\\leq2$ or $\\beta\\leq1$. The second contribution isto determine the maximum order of a graph in $\\mathcal{G}_{\\beta,D}$ for allvalues of $D$ and $\\beta$. Only a weak upper bound was previously known.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We consider a system composed of a trapped atom and a trapped ion. The ioncharge induces in the atom an electric dipole moment, which attracts it with anr^{-4} dependence at large distances. In the regime considered here, thecharacteristic range of the atom-ion interaction is comparable or larger thanthe characteristic size of the trapping potential, which excludes theapplication of the contact pseudopotential. The short-range part of theinteraction is described in the framework of quantum-defect theory, byintroducing some short-range parameters, which can be related to the s-wavescattering length. When the separation between traps is changed we observetrap-induced shape resonances between molecular bound states and vibrationalstates of the external trapping potential. Our analysis is extended toquasi-one-dimensional geometries, when the scattering exhibitconfinement-induced resonances, similar to the ones studied before forshort-range interactions. For quasi-one-dimensional systems we investigate theeffects of coupling between the center of mass and relative motion, whichoccurs for different trapping frequencies of atom and ion traps. Finally, weshow how the two types of resonances can be employed for quantum state controland spectroscopy of atom-ion molecules.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We theoretically demonstrate the formation of multiple bi-stability regionsin the temperature pattern on the interface between a cuprous oxide quantumwell and DCM2:CA:PS organic compound. The Frenkel molecular exciton of the DCM2is brought into resonance with the $1S$ quadrupole Wannier-Mott exciton in thecuprous oxide by \"solvatochromism\" with CA. The resulting hybrid is thermalizedwith surrounding helium bath. This leads to strongly non-linear temperaturedependence of the laser field detuning from the quadrupole exciton energy bandwhich is associated with the temperature induced red shift of the Wannierexciton energy. Numerical up and down-scan for the detuning revealshysteresis-like temperature distribution. The obtained \\emph{multiple}bi-stability regions are at least three orders of magnitude bigger ($meV$) thanthe experimentally observed bi-stability in bulk cuprous oxide ($\\mu eV$). Theeffective absorption curve exhibits highly asymmetrical behavior for theFrenkel-like (above the $1S$ energy) and Wannier-like (below the $1S$ energy)branches of the hybrid.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The intrinsic distribution of spectral indices in GeV energies ofgamma-ray--loud blazars is a critical input in determining the spectral shapeof the unresolved blazar contribution to the diffuse extragalactic gamma-raybackground, as well as an important test of blazar emission theories. Wepresent a maximum-likelihood method of determining the intrinsic spectral indexdistribution (ISID) of a population of gamma-ray emitters which accounts forerror in measurement of individual spectral indices, and we apply it to EGRETblazars. We find that the most likely Gaussian ISID for EGRET blazars has amean of 2.27 and a standard deviation of 0.20. We additionally find someindication that FSRQs and BL Lacs may have different ISIDs (with BL Lacs beingharder). We also test for spectral index hardening associated with blazarvariability for which we find no evidence. Finally, we produce simulated GLASTspectral index datasets and perform the same analyses. With improved statisticsdue to the much larger number of resolvable blazars, GLAST data will help usdetermine the ISIDs with much improved accuracy. Should any difference existbetween the ISIDs of BL Lacs and FSRQs or between the ISIDs of blazars in thequiescent and flaring states, GLAST data will be adequate to separate theseISIDs at a significance better than 3 sigma.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We study by extensive Monte Carlo simulations the transport of itinerantspins travelling inside a multilayer composed of three ferromagnetic filmsantiferromagnetically coupled to each other in a sandwich structure. The twoexterior films interact with the middle one through non magnetic spacers. Thespin model is the Ising one and the in-plane transport is considered. Variousinteractions are taken into account. We show that the current of the itinerantspins going through this system depends strongly on the magnetic ordering ofthe multilayer: at temperatures $T$ below (above) the transition temperature$T_c$, a strong (weak) current is observed. This results in a strong jump ofthe resistance across $T_c$. Moreover, we observe an anomalous variation,namely a peak, of the spin current in the critical region just above $T_c$. Weshow that this peak is due to the formation of domains in the temperatureregion between the low-$T$ ordered phase and the true paramagnetic disorderedphase. The existence of such domains is known in the theory of criticalphenomena. The behavior of the resistance obtained here is compared to a recentexperiment. An excellent agreement with our physical interpretation isobserved. We also show and discuss effects of various physical parametersentering our model such as interaction range, strength of electric and magneticfields and magnetic film and non magnetic spacer thicknesses.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Using data recorded by the Michelson Doppler Imager (MDI) instrument on theSolar and Heliospheric Observatory (SOHO), we have traced 123 pairs of oppositemagnetic polarity moving magnetic features (MMFs) in three active regions NOAAARs 8375, 0330 and 9575. At the time of observation, AR 8375 was young, AR 0330mature, and AR 9575 decaying. The vertical velocity indicates that the elementsof MMF pairs with polarity opposite to that of the sunspot support a downflowof around 50-100 m s$^{-1}$. The average Doppler shift difference betweennegative and positive elements of an MMF pair is about 150 m s$^{-1}$ in AR8375, 100 m s$^{-1}$ in AR 0330, and 20 m s$^{-1}$ in AR 9575. Theseobservational results are in agreement with the model that MMF pairs are partof a U-loop emanating from the sunspot's magnetic canopy. According to thismodel the downflow is caused by the Evershed flow returning below the solarsurface. For AR 8375, the horizontal velocity of MMFs ranges from 0.1 kms$^{-1}$ to 0.7 km s$^{-1}$, and on average, the velocity of an MMF pairdecreases significantly (from 0.6 km s$^{-1}$ to 0.35 km s$^{-1}$) withincreasing distance from the MMF's birth place. This result suggests that thechange in MMF flow speed does not reflect the radial structure of the moatflow, but rather is intrinsic to the evolution of the MMF pairs. This result isalso in agreement with the U-loop model of MMF pairs. We also find thatproperties of MMF pairs, most strikingly the lifetime, depend on the evolutionstages of the parent sunspot. The mean lifetimes of MMF pairs in ARs 9575 and0330 are 0.7 hours and 1.6 hours, respectively, which is considerably shorterthan the 4 hours lifetime previously found for AR 8375.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We report the measurement of extremely slow hole spin relaxation dynamics insmall ensembles of self-assembled InGaAs quantum dots. Individual spinorientated holes are optically created in the lowest orbital state of each dotand read out after a defined storage time using spin memory devices. Theresulting luminescence signal exhibits a pronounced polarization memory effectthat vanishes for long storage times. The hole spin relaxation dynamics aremeasured as a function of external magnetic field and lattice temperature. Weshow that hole spin relaxation can occur over remarkably long timescales instrongly confined quantum dots (up to ~270 us), as predicted by recent theory.Our findings are supported by calculations that reproduce both the observedmagnetic field and temperature dependencies. The results suggest that hole spinrelaxation in strongly confined quantum dots is due to spin orbit mediatedphonon scattering between Zeeman levels, in marked contrast to higherdimensional nanostructures where it is limited by valence band mixing.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Supermassive black hole binary (SMBHB) is expected with the hierarchicalgalaxy formation model. Currently, physics processes dominating the evolutionof a SMBHB are unclear. An interesting question is whether we couldobservationally determine the evolution of SMBHB and give constraints on thephysical processes. Jet precession have been observed in many AGNs andgenerally attributed to disk precession. In this paper we calculate the timevariation of jet precession and conclude that jet precession is accelerated inSMBHB systems but decelerated in others. The acceleration of jet precession$dP_{\\rm pr} / dt$ is related to jet precession timescale $P_{\\rm pr}$ andSMBHB evolution timescale $\\tau_{\\rm a}$, ${dP_{\\rm pr} \\over dt} \\simeq -\\Lambda {P_{\\rm pr} \\over \\tau_{\\rm a}}$. Our calculations based on the modelsfor jet precession and SMBHB evolution show that $dP_{\\rm pr} / dt$ can be ashigh as about $- 1.0$ with a typical value -0.2 and can be easily detected. Wediscussed the differential jet precession for NGC1275 observed in theliterature. If the observed rapid acceleration of jet precession is true, thejet precession is due to the orbital motion of an unbound SMBHB with mass ratio$q\\approx 0.76$. When jets precessed from the ancient bubbles to the currentlyactive jets, the separation of SMBHB decrease from about $1.46 {\\rm Kpc}$ to$0.80 {\\rm Kpc}$ with an averaged decreasing velocity $da/dt \\simeq - 1.54\\times 10^6 {\\rm cm/s}$ and evolution timescale $\\tau_{\\rm a} \\approx 7.5\\times10^7 {\\rm yr}$. However, if we assume a steady jet precession for many cycles,the observations implies a hard SMBHB with mass ratio $q\\approx 0.21$ andseparation $a\\approx 0.29 {\\rm pc}$.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Active galactic nuclei, x-ray binaries, pulsars, and gamma-ray bursts are allbelieved to be powered by compact objects surrounded by relativistic plasmaflows driving phenomena such as accretion, winds, and jets. These flows areoften accurately modelled by the relativistic magnetohydrodynamics (MHD)approximation. Time-dependent numerical MHD simulations have proven to beespecially insightful, but one regime that remains difficult to simulate iswhen the energy scales (kinetic, thermal, magnetic) within the plasma becomedisparate. We develop a numerical scheme that significantly improves theaccuracy and robustness of the solution in this regime. We use a modified formof the WENO method to construct a finite-volume general relativistichydrodynamics code called WHAM that converges at fifth order. We avoid (1)field-by-field decomposition by adaptively reducing down to 2-point stencilsnear discontinuities for a more accurate treatment of shocks, and (2) excessivereduction to low order stencils, as in the standard WENO formalism, bymaintaining high order accuracy in smooth monotonic flows. Our scheme performsthe proper surface integral of the fluxes, converts cell averaged conservedquantities to point conserved quantities before performing the reconstructionstep, and correctly averages all source terms. We demonstrate that the schemeis robust in strong shocks, very accurate in smooth flows, and maintainsaccuracy even when the energy scales in the flow are highly disparate.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Many extra-solar planets discovered over the past decade are gas giants intight orbits around their host stars. Due to the difficulties of forming these`hot Jupiters' in situ, they are generally assumed to have migrated to theirpresent orbits through interactions with their nascent discs. In this paper, wepresent a systematic study of giant planet migration in power law discs. Wefind that the planetary migration rate is proportional to the disc surfacedensity. This is inconsistent with the assumption that the migration rate issimply the viscous drift speed of the disc. However, this result can beobtained by balancing the angular momentum of the planet with the viscoustorque in the disc. We have verified that this result is not affected byadjusting the resolution of the grid, the smoothing length used, or the time atwhich the planet is released to migrate.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Inelastic effects in the Coulomb blockade and Kondo regimes of electrontransport through molecular junctions are considered within a simplenonequilibrium equation-of-motion (EOM) approach. The scheme isself-consistent, and can qualitatively reproduce the main experimentalobservations of vibrational features in Coulomb blockade [H.Park et al., Nature407, 57 (2000)] and Kondo [L.H.Yu et al., Phys. Rev. Lett. 93, 266802 (2004)]regimes. Considerations similar to the equilibrium EOM approach by Meir et al.[Phys. Rev. Lett. 66, 3048 (1991); ibid. 70, 2601 (1993)] are used on theKeldysh contour to account for the nonequilibrium nature of the junction, anddressing by appropriate Franck-Condon (FC) factors is used to account forvibrational features. Results of the equilibrium EOM scheme by Meir et al. arereproduced in the appropriate limit.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Vacuum expectation values of the field square and the energy-momentum tensorfor the electromagnetic field are investigated for the geometry of a wedge witha coaxal cylindrical boundary. All boundaries are assumed to be perfectlyconducting and both regions inside and outside the shell are considered. Byusing the generalized Abel-Plana formula, the vacuum expectation values arepresented in the form of the sum of two terms. The first one corresponds to thegeometry of the wedge without the cylindrical shell and the second term isinduced by the presence of the shell. The vacuum energy density induced by theshell is negative for the interior region and is positive for the exteriorregion. The asymptotic behavior of the vacuum expectation values areinvestigated in various limiting cases. It is shown that the vacuum forcesacting on the wedge sides due to the presence of the cylindrical boundary arealways attractive.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present results from an analysis of B0 to rho+rho- decays using 383.6million BB-bar pairs collected by the BaBar detector at the PEP-IIasymmetric-energy B Factory at SLAC. The measurements of the B0 to rho+rho-branching fraction, longitudinal polarization fraction f_L, and theCP-violating parameters S_{long} and C_{long} are:  B(B0-> rho+rho-) = (25.5 +/- 2.1 (stat) +3.6/-3.9 (syst))*10^-6 f_L = 0.992+/- 0.024 (stat) +0.026/-0.013 (syst) S_{long} = -0.17 +/- 0.20 (stat)+0.05/-0.06 (syst) C_{long} = 0.01 +/- 0.15 (stat) +/- 0.06 (syst) We determinethe unitarity triangle angle alpha, using an isospin analysis of B to rhorhodecays. One of the two solutions, alpha = [73.1, 117.0] degrees at 68% CL iscompatible with standard model-based fits of existing data. Constraints on theunitarity triangle are also evaluated using an SU(3) symmetry based approach.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Sunspot penumbrae show a fine structure in continuum intensity that displaysconsiderable dynamics. The magnetic field, in contrast, although also highlystructured, has appeared to be relatively static. Here we report the discoveryof inward moving magnetic enhancements in the penumbrae of two regular sunspotsbased on time series of SOHO/MDI magnetograms. Local enhancements of the LOScomponent of the magnetic field in the inner part of the penumbral region moveinward to the umbra-penumbra boundary with a radial speed of about 0.3 kms$^{-1}$. These local inward-moving enhancements of the LOS component of themagnetic fields appear to be relatively common. They are associated with darkstructures and tend to display downflows relatively to the penumbralbackground. Possible explanations are discussed.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We introduce the straggler identification problem, in which an algorithm mustdetermine the identities of the remaining members of a set after it has had alarge number of insertion and deletion operations performed on it, and now hasrelatively few remaining members. The goal is to do this in o(n) space, where nis the total number of identities. The straggler identification problem hasapplications, for example, in determining the set of unacknowledged packets ina high-bandwidth multicast data stream. We provide a deterministic solution tothe straggler identification problem that uses only O(d log n) bits and isbased on a novel application of Newton's identities for symmetric polynomials.This solution can identify any subset of d stragglers from a set of n O(logn)-bit identifiers, assuming that there are no false deletions of identitiesnot already in the set. Indeed, we give a lower bound argument that shows thatany small-space deterministic solution to the straggler identification problemcannot be guaranteed to handle false deletions. Nevertheless, we show thatthere is a simple randomized solution using O(d log n log(1/epsilon)) bits thatcan maintain a multiset and solve the straggler identification problem,tolerating false deletions, where epsilon>0 is a user-defined parameterbounding the probability of an incorrect response. This randomized solution isbased on a new type of Bloom filter, which we call the invertible Bloom filter.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We propose two novel experiments on the measurement of the Casimir forceacting between a gold coated sphere and semiconductor plates with markedlydifferent charge carrier densities. In the first of these experiments apatterned Si plate is used which consists of two sections of different dopantdensities and oscillates in the horizontal direction below a sphere. Themeasurement scheme in this experiment is differential, i.e., allows the directhigh-precision measurement of the difference of the Casimir forces between thesphere and sections of the patterned plate or the difference of the equivalentpressures between Au and patterned parallel plates with static and dynamictechniques, respectively. The second experiment proposes to measure the Casimirforce between the same sphere and a VO${}_2$ film which undergoes theinsulator-metal phase transition with the increase of temperature. We reportthe present status of the interferometer based variable temperature apparatusdeveloped to perform both experiments and present the first results on thecalibration and sensitivity. The magnitudes of the Casimir forces and pressuresin the experimental configurations are calculated using different theoreticalapproaches to the description of optical and conductivity properties ofsemiconductors at low frequencies proposed in the literature. It is shown thatthe suggested experiments will aid in the resolution of theoretical problemsarising in the application of the Lifshitz theory at nonzero temperature toreal materials. They will also open new opportunities in nanotechnology.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We provide a new algorithm for the treatment of inverse problems whichcombines the traditional SVD inversion with an appropriate thresholdingtechnique in a well chosen new basis. Our goal is to devise an inversionprocedure which has the advantages of localization and multiscale analysis ofwavelet representations without losing the stability and computability of theSVD decompositions. To this end we utilize the construction of localized frames(termed \"needlets\") built upon the SVD bases. We consider two differentsituations: the \"wavelet\" scenario, where the needlets are assumed to behavesimilarly to true wavelets, and the \"Jacobi-type\" scenario, where we assumethat the properties of the frame truly depend on the SVD basis at hand (henceon the operator). To illustrate each situation, we apply the estimationalgorithm respectively to the deconvolution problem and to the Wicksellproblem. In the latter case, where the SVD basis is a Jacobi polynomial basis,we show that our scheme is capable of achieving rates of convergence which areoptimal in the $L_2$ case, we obtain interesting rates of convergence for other$L_p$ norms which are new (to the best of our knowledge) in the literature, andwe also give a simulation study showing that the NEED-D estimator outperformsother standard algorithms in almost all situations.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "It has been recently argued through numerical work that rotating stars with ahigh degree of differential rotation are dynamically unstable against bar-modedeformation, even for values of the ratio of rotational kinetic energy togravitational potential energy as low as O(0.01). This may have implicationsfor gravitational wave astronomy in high-frequency sources such as corecollapse supernovae. In this paper we present high-resolution simulations,performed with an adaptive mesh refinement hydrodynamics code, of such lowT/|W| bar-mode instability. The complex morphological features involved in thenonlinear dynamics of the instability are revealed in our simulations, whichshow that the excitation of Kelvin-Helmholtz-like fluid modes outside thecorotation radius of the star leads to the saturation of the bar-modedeformation. While the overall trends reported in an earlier investigation areconfirmed by our work, we also find that numerical resolution plays animportant role during the long-term, nonlinear behaviour of the instability,which has implications on the dynamics of rotating stars and on the attainableamplitudes of the associated gravitational wave signals.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "A free zero-range process (FRZP) is a simple stochastic process describingthe dynamics of a gas of particles hopping between neighboring nodes of anetwork. We discuss three different cases of increasing complexity: (a) FZRP ona rigid geometry where the network is fixed during the process, (b) FZRP on arandom graph chosen from a given ensemble of networks, (c) FZRP on a dynamicalnetwork whose topology continuously changes during the process in a way whichdepends on the current distribution of particles. The case (a) provides a verysimple realization of the phenomenon of condensation which manifests as theappearance of a condensate of particles on the node with maximal degree. Thecase (b) is very interesting since the averaging over typical ensembles ofgraphs acts as a kind of homogenization of the system which makes all nodesidentical from the point of view of the FZRP. In the case (c), the distributionof particles and the dynamics of network are coupled to each other. Thestrength of this coupling depends on the ratio of two time scales: for changesof the topology and of the FZRP. We will discuss a specific example of thattype of interaction and show that it leads to an interesting phase diagram.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Mass loss rate formulae are derived from observations or from suites ofmodels. For theoretical models, the following have all been identified asfactors greatly influencing the atmospheric structure and mass loss rates:Pulsation with piston amplitude scaling appropriately with stellar L; dustnucleation and growth, with radiation pressure and grain-gas interactions andappropriate dependence on temperature and density; non-grey opacity with atleast 51 frequency samples; non-LTE and departures from radiative equilibriumin the compressed and expanding flows; and non-equilibrium processes affectingthe composition (grain formation; molecular chemistry). No one set of modelsyet includes all the factors known to be important. In fact, it is verydifficult to construct a model that can simultaneously include these factorsand be useful for computing spectra. Therefore, although theoretical modelgrids are needed to separate the effects of M,L,R and/or $T_{\\mathrm{eff}}$ orZ on the mass loss rates, these models must be carefully checked againstobservations. Getting the right order of magnitude for the mass loss rate isonly the first step in such a comparison, and is not sufficient to determinewhether the mass loss formula is correct. However, there are observables thatdo test the validity of mass loss formulae as they depend directly on $d\\log\\dot M/d\\log L$, $d\\log \\dot M/d\\log R$, or $d\\log \\dot M/d\\log P$.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Qualitatively new aspects of the (linear and non-linear) stability of shearedrelativistic (slab) jets are analyzed. The linear problem has been solved for awide range of jet models well inside the ultrarelativistic domain (flow Lorentzfactors up to 20; specific internal energies $\\approx 60c^2$). As a distinctfeature of our work, we have combined the analytical linear approach withhigh-resolution relativistic hydrodynamical simulations, which has allowed usi) to identify, in the linear regime, resonant modes specific to therelativistic shear layer ii) to confirm the result of the linear analysis withnumerical simulations and, iii) more interestingly, to follow the instabilitydevelopment through the non-linear regime. We find that very high-orderreflection modes with dominant growth rates can modify the global, long-termstability of the relativistic flow. We discuss the dependence of these resonantmodes on the jet flow Lorentz factor and specific internal energy, and on theshear layer thickness. The results could have potential applications in thefield of extragalactic relativistic jets.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Substantial collective flow is observed in collisions between large nuclei athigh energy, as evidenced by single-particle transverse momentum distributionsand by azimuthal correlations among the produced particles. The data arewell-reproduced by perfect fluid dynamics. In a separate development,calculation of the dimensionless ratio of shear viscosity eta to entropydensity s by Kovtun, Son and Starinets within AdS/CFT yields eta/s = 1/4pi, andthey conjectured that this is a lower bound for any physical system. It isshown that the transition from hadrons to quarks and gluons has behaviorsimilar to helium, nitrogen, and water at and near their phase transitions inthe ratio eta/s. Therefore it is possible that experimental measurements canpinpoint the location of this transition or rapid crossover in QCD via theviscosity to entropy ratio in addition to and independently of the equation ofstate.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The LHC will have unprecedented sensitivity to flavor-changing neutralcurrent (FCNC) top quark decays, whose observation would be a clear sign ofphysics beyond the standard model. Although many details of top flavorviolation are model dependent, the standard model gauge symmetries relate topFCNCs to other processes, which are strongly constrained by existing data. Westudy these constraints in a model independent way, using a low energyeffective theory from which the new physics is integrated out. We consider themost important operators which contribute to top FCNCs and analyze the currentconstraints on them. We find that the data rule out top FCNCs at a levelobservable at the LHC due to most of the operators comprising left-handed firstor second generation quark fields, while there remains a substantial window fortop decays mediated by operators with right-handed charm or up quarks. If FCNCtop decays are observed at the LHC, such an analysis may help decipher theunderlying physics.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We address the problem of constructing high-accuracy, faithful analyticwaveforms describing the gravitational wave signal emitted by inspiralling andcoalescing binary black holes. We work within the Effective-One-Body (EOB)framework and propose a methodology for improving the current(waveform)implementations of this framework based on understanding, element byelement, the physics behind each feature of the waveform, and on systematicallycomparing various EOB-based waveforms with ``exact'' waveforms obtained bynumerical relativity approaches. The present paper focuses on small-mass-rationon-spinning binary systems, which can be conveniently studied byRegge-Wheeler-Zerilli-type methods. Our results include: (i) a resummed,3PN-accurate description of the inspiral waveform, (ii) a better description ofradiation reaction during the plunge, (iii) a refined analytic expression forthe plunge waveform, (iv) an improved treatment of the matching between theplunge and ring-down waveforms. This improved implementation of the EOBapproach allows us to construct complete analytic waveforms which exhibit aremarkable agreement with the ``exact'' ones in modulus, frequency and phase.In particular, the analytic and numerical waveforms stay in phase, during thewhole process, within $\\pm 1.1 %$ of a cycle. We expect that the extension ofour methodology to the comparable-mass case will be able to generate comparablyaccurate analytic waveforms of direct use for the ground-based network ofinterferometric detectors of gravitational waves.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We have carried out neutron powder-diffraction measurements on zincparatacamite Zn$_x$Cu$_{4-x}$(OH)$_6$Cl$_2$ with $x=1$, and studied the heatcapacity in fields of up to 9 T for $0.5 \\leq x \\leq 1$. The $x=1$ phase hasrecently been shown to be an outstanding realisation of the $S=1/2$ kagom\\'{e}antiferromagnet. A weak mixing of Cu$^{2+}$/Zn$^{2+}$ between the Cu and the Znsites, corresponding to $\\sim 9$% of all Cu$^{2+}$ for $x=1$, is observed usingneutron diffraction. This ``antisite disorder'' provides a consistentexplanation of the field dependence of the heat capacity for $0.8 \\leq x \\leq1$. From comparison of the derived Cu$^{2+}$ occupancy of the Zn sites for $x =0.8... 1$ with the magnetic susceptibility, we argue that for $x = 0.8... 1$zinc paratacamite is a spin liquid without a spin gap. The presence of unpairedbut nevertheless strongly interacting spins gives rise to a macroscopicallydegenerate ground state manifold, with increasingly glassy dynamics as $x$ islowered.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Single-particle excitation spectra of the two-dimensional Hubbard model onthe square lattice near half filling and at zero temperature are investigatedon the basis of the self-consistent projection operator method. The methodguarantees a high accuracy of the spectra with high energy and high momentumresolutions. It takes into account long-range intersite correlations as well asthe strong on-site correlations. Effects of nonlocal excitations are clarifiedby comparing the results with those of the single-site approximation. Thecalculated spectra verify the quantum Monte-Carlo results for finitetemperatures. The spectra at the Fermi level yield a hole-like Fermi surface inthe underdoped region and an electron-like Fermi surface in the overdopedregion. From a numerical analysis of the momentum dependent effective mass andself-energy, it is concluded that a marginal Fermi-liquid like state persistseven at finite doping concentrations in the strongly correlated region becausea van Hove singularity is pinned to the Fermi surface. It is also found that akink structure appears in the quasiparticle energy band in the same region. Thekink is shown to be caused by a mixing between the quasiparticle band and anexcitation band with strong short-range antiferromagnetic correlations. Theseresults suggest an explanation for some of the unusual properties of the normalstate in high-$T_{\\rm c}$ cuprates.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We show that dynamical relaxation in the aftermath of a galactic merger andthe ensuing formation and decay of a binary massive black hole (MBH), aredominated by massive perturbers (MPs) such as giant molecular clouds orclusters. MPs accelerate relaxation by orders of magnitude relative to 2-bodystellar relaxation alone, and efficiently scatter stars into the binary MBH'sorbit. The 3-body star-binary MBH interactions shrink the binary MBH to thepoint where energy losses from the emission of gravitational waves (GW) lead torapid coalescence. We model this process based on observed and simulated MPdistributions and take into account the decreased efficiency of the star-binaryMBH interaction due to acceleration in the galactic potential. We show thatmergers of gas-rich galactic nuclei lead to binary MBH coalescence well withinthe Hubble time. Moreover, lower-mass binary MBHs (<10^8 Msun) require only afew percent of the typical gas mass in a post-merger nucleus to coalesce in aHubble time. The fate of a binary MBH in a gas poor galactic merger is lesscertain, although massive stellar structures (e.g. clusters, stellar rings)could likewise lead to efficient coalescence. These coalescence events areobservable by their strong GW emission. MPs thus increase the cosmic rate ofsuch GW events, lead to a higher mass deficit in the merged galactic core andsuppress the formation of triple MBH systems and the resulting ejection of MBHsinto intergalactic space.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We generalize and greatly simplify the approach of Lydakis andDundas-R\\\"ondigs-{\\O}stv{\\ae}r to construct an L-stable model structure forsmall functors from a closed symmetric monoidal model category V to a V-modelcategory M, where L is a small cofibrant object of V. For the special caseV=M=S_* pointed simplicial sets and L=S^1 this is the classical case of linearfunctors and has been described as the first stage of the Goodwillie tower of ahomotopy functor. We show, that our various model structures are compatiblewith a closed symmetric monoidal product on small functors. We compare themwith other L-stabilizations described by Hovey, Jardine and others. This givesa particularly easy construction of the classical and the motivic stablehomotopy category with the correct smash product. We establish the monoid axiomunder certain conditions.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We analyse high-time-resolution spectroscopy of the AM CVn stars HP Libraeand V803 Centauri, taken with the New Technology Telescope (NTT) and the VeryLarge Telescope (VLT) of the European Southern Observatory, Chile.  We present evidence that the literature value for V803 Cen's orbital periodis incorrect, based on an observed `S-wave' in the binary's spectrogram. Wemeasure a spectroscopic period P=1596.4+/-1.2s of the S-wave feature, which issignificantly shorter than the 1611-second periods found in previousphotometric studies. We conclude that the latter period likely represents a`superhump'. If one assumes that our S-wave period is the orbital period, V803Cen's mass ratio can be expected to be much less extreme than previouslythought, at q~0.07 rather than q~0.016. This relaxes the constraints on themasses of the components considerably: the donor star does then not need to befully degenerate, and the mass of the accreting white dwarf no longer has to bevery close to the Chandrasekhar limit.  For HP Lib, we similarly measure a spectroscopic period P=1102.8+/-0.2s. Thissupports the identification of HP Lib's photometric periods found in theliterature, and the constraints upon the masses derived from them.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Thermally stimulated luminescence (TSL) and conductivity (TSC) are consideredusing the classical insulator model that assumes one kind of the active trap,one kind of inactive deep trap, and one kind of the recombination center.Kinetic equations describing the model are solved numerically without and withthe use of the quasiequilibrium (QE) approximation. The QE state parameter qI,,the relative recombination probability g, and a new parameter calledquasi-stationary (QS) state parameter q*=qIg are used for the analysis of theTSL and TSC. The TSL and TSC curves and the temperature dependences of qI, q*,g, the recombination lifetime, and the occupancies of active traps andrecombination centers are numerically calculated for five sets of kineticparameters and different heating rates. These calculation results show that:(1) the upper limit of the heating rate for presence of the QS state appears athigher heating rate than that for the QE state when the retrapping process ispresent, and (2) the TSL (TSC) curves in the QS state have the propertiessimilar to those for the TSL (TSC) curves in the QE state. Approximate formulasfor calculation of the parameters qI and q* in the initial range of the TSL andTSC curves are derived and used in the heating-rate methods, proposed in thiswork, for determination of those parameters from the calculated TSL curves.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "A charge injection technique is applied to the X-ray CCD camera, XIS (X-rayImaging Spectrometer) onboard Suzaku. The charge transfer inefficiency (CTI) ineach CCD column (vertical transfer channel) is measured by the injection ofcharge packets into a transfer channel and subsequent readout. This paperreports the performances of the charge injection capability based on the groundexperiments using a radiation damaged device, and in-orbit measurements of theXIS. The ground experiments show that charges are stably injected with thedispersion of 91eV in FWHM in a specific column for the charges equivalent tothe X-ray energy of 5.1keV. This dispersion width is significantly smaller thanthat of the X-ray events of 113eV (FWHM) at approximately the same energy. Theamount of charge loss during transfer in a specific column, which is measuredwith the charge injection capability, is consistent with that measured with thecalibration source. These results indicate that the charge injection techniquecan accurately measure column-dependent charge losses rather than thecalibration sources. The column-to-column CTI correction to the calibrationsource spectra significantly reduces the line widths compared to those with acolumn-averaged CTI correction (from 193eV to 173eV in FWHM on an average atthe time of one year after the launch). In addition, this method significantlyreduces the low energy tail in the line profile of the calibration sourcespectrum.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The present paper introduces an original biofeedback system for improvinghuman balance control, whose underlying principle consists in providingadditional sensory information related to foot sole pressure distribution tothe user through a tongue-placed tactile output device. To assess the effect ofthis biofeedback system on postural control during quiet standing, ten younghealthy adults were asked to stand as immobile as possible with their eyesclosed in two conditions of No-biofeedback and Biofeedback. Centre of footpressure (CoP) displacements were recorded using a force platform. Resultsshowed reduced CoP displacements in the Biofeedback relative to theNo-biofeedback condition. The present findings evidenced the ability of thecentral nervous system to efficiently integrate an artificial plantar-based,tongue-placed tactile biofeedback for controlling control posture during quietstanding.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Shor's powerful quantum algorithm for factoring represents a major challengein quantum computation and its full realization will have a large impact onmodern cryptography. Here we implement a compiled version of Shor's algorithmin a photonic system using single photons and employing the non-linearityinduced by measurement. For the first time we demonstrate the core processes,coherent control, and resultant entangled states that are required in afull-scale implementation of Shor's algorithm. Demonstration of these processesis a necessary step on the path towards a full implementation of Shor'salgorithm and scalable quantum computing. Our results highlight that theperformance of a quantum algorithm is not the same as performance of theunderlying quantum circuit, and stress the importance of developing techniquesfor characterising quantum algorithms.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Security of information has become a major issue during the last decades. Newalgorithms based on chaotic maps were suggested for protection of differenttypes of multimedia data, especially digital images and videos in this period.However, many of them fundamentally were flawed by a lack of robustness andsecurity. For getting higher security and higher complexity, in the currentpaper, we introduce a new kind of symmetric key block cipher algorithm that isbased on \\emph{tripled chaotic maps}. In this algorithm, the utilization of twocoupling parameters, as well as the increased complexity of the cryptosystem,make a contribution to the development of cryptosystem with higher security. Inorder to increase the security of the proposed algorithm, the size of key spaceand the computational complexity of the coupling parameters should be increasedas well. Both the theoretical and experimental results state that the proposedalgorithm has many capabilities such as acceptable speed and complexity in thealgorithm due to the existence of two coupling parameter and high security.Note that the ciphertext has a flat distribution and has the same size as theplaintext. Therefore, it is suitable for practical use in securecommunications.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The ability to control the conductance of single molecules will have a majorimpact in nanoscale electronics. Azobenzene, a molecule that changesconformation as a result of a trans/cis transition when exposed to radiation,could form the basis of a light-driven molecular switch. It is thereforecrucial to clarify the electrical transport characteristics of this molecule.Here, we investigate theoretically charge transport in a system in which asingle azobenzene molecule is attached to two carbon nanotubes. In clearcontrast to gold electrodes, the nanotubes can act as true nanoscale electrodesand we show that the low-energy conduction properties of the junction may bedramatically modified by changing the topology of the contacts between thenanotubes and the molecules, and/or the chirality of the nanotubes (that is,zigzag or armchair). We propose experiments to demonstrate controlledelectrical switching with nanotube electrodes.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "An efficient quantum cryptography network protocol is proposed withd-dimension polarized photons, without resorting to entanglement and quantummemory. A server on the network, say Alice, provides the service for preparingand measuring single photons whose initial state are |0>. The users code theinformation on the single photons with some unitary operations. For preventingthe untrustworthy server Alice from eavesdropping the quantum lines, anonorthogonal-coding technique (decoy-photon technique) is used in the processthat the quantum signal is transmitted between the users. This protocol doesnot require the servers and the users to store the quantum state and almost allof the single photons can be used for carrying the information, which makes itmore convenient for application than others with present technology. We alsodiscuss the case with a faint laser pulse.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We study the population of satellite galaxies formed in a suite ofN-body/gasdynamical simulations of galaxy formation in a LCDM universe. We findlittle spatial or kinematic bias between the dark matter and the satellitepopulation. The velocity dispersion of the satellites is a good indicator ofthe virial velocity of the halo: \\sigma_{sat}/V_{vir}=0.9 +/- 0.2. Applied tothe Milky Way and M31 this gives V_{vir}^{MW}=109 +/- 22$ km/s andV_{vir}^{M31} = 138 +/- 35 km/s, respectively, substantially lower than therotation speed of their disk components. The detailed kinematics of simulatedsatellites and dark matter are also in good agreement. By contrast, the stellarhalo of the simulated galaxies is kinematically and spatially distinct from thepopulation of surviving satellites. This is because the survival of a satellitedepends on mass and on time of accretion; surviving satellites are biasedtoward low-mass systems that have been recently accreted by the galaxy. Ourresults support recent proposals for the origin of the systematic differencesbetween stars in the Galactic halo and in Galactic satellites: the elusive``building blocks'' of the Milky Way stellar halo were on average more massive,and were accreted (and disrupted) earlier than the population of dwarfs thathas survived self-bound until the present.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "In time hopping impulse radio, $N_f$ pulses of duration $T_c$ are transmittedfor each information symbol. This gives rise to two types of processing gain:(i) pulse combining gain, which is a factor $N_f$, and (ii) pulse spreadinggain, which is $N_c=T_f/T_c$, where $T_f$ is the mean interval between twosubsequent pulses. This paper investigates the trade-off between these twotypes of processing gain in the presence of timing jitter. First, an additivewhite Gaussian noise (AWGN) channel is considered and approximate closed formexpressions for bit error probability are derived for impulse radio systemswith and without pulse-based polarity randomization. Both symbol-synchronousand chip-synchronous scenarios are considered. The effects of multiple-accessinterference and timing jitter on the selection of optimal system parametersare explained through theoretical analysis. Finally, a multipath scenario isconsidered and the trade-off between processing gains of a synchronous impulseradio system with pulse-based polarity randomization is analyzed. The effectsof the timing jitter, multiple-access interference and inter-frame interferenceare investigated. Simulation studies support the theoretical results.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The scaling behaviors of graphene nanoribbon (GNR) Schottky barrierfield-effect transistors (SBFETs) are studied by solving the non-equilibriumGreen's function (NEGF) transport equation in an atomistic basis setself-consistently with a three-dimensional Poisson equation. The armchair edgeGNR channel shares similarities with a zigzag CNT, but it has a differentgeometry and quantum confinement boundary condition in the transversedirection. The results indicate that the I-V characteristics are ambipolar andstrongly depend on the GNR width because the bandgap of the GNR isapproximately inversely proportional to its width, which agrees with recentexperiments. A multiple gate geometry improves immunity to short channeleffects, but it offers smaller improvement than it does for Si MOSFETs in termsof the on-current and transconductance. Reducing the oxide thickness is moreuseful for improving transistor performance than using a high-k gate insulator.Significant increase of the minimal leakage current is observed when thechannel length is scaled below 10nm because the small effective massfacilitates strong source-drain tunneling. The GNRFET, therefore, does notpromise extending the ultimate scaling limit of Si MOSFETs. The intrinsicswitching speed of a GNR SBFET, however, is several times faster than that ofSi MOSFETs, which could lead to promising high speed electronics applications,where the large leakage of GNR SBFETs is of less concern.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Since its discovery in the 1930s, the muon has played an important role inour quest to understand the sub-atomic theory of matter. The muon was the firstsecond-generation standard-model particle to be discovered, and its decay hasprovided information on the (Vector -Axial Vector) structure of the weakinteraction, the strength of the weak interaction, G_F, and the conservation oflepton number (flavor) in muon decay. The muon's anomalous magnetic moment hasplayed an important role in restricting theories of physics beyond the standardstandard model, where at present there is a 3.4 standard-deviation differencebetween the experiment and standard-model theory. Its capture on the atomicnucleus has provided valuable information on the modification of the weakcurrent by the strong interaction which is complementary to that obtained fromnuclear beta decay.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "This paper presents the principles of ontology-supported and ontology-drivenconceptual navigation. Conceptual navigation realizes the independence betweenresources and links to facilitate interoperability and reusability. An enginebuilds dynamic links, assembles resources under an argumentative scheme andallows optimization with a possible constraint, such as the user's availabletime. Among several strategies, two are discussed in detail with examples ofapplications. On the one hand, conceptual specifications for linking andassembling are embedded in the resource meta-description with the support ofthe ontology of the domain to facilitate meta-communication. Resources are likeagents looking for conceptual acquaintances with intention. On the other hand,the domain ontology and an argumentative ontology drive the linking andassembling strategies.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We report infrared photometry of the extrasolar planet HD 209458b during thetime of secondary eclipse (planet passing behind the star). Observations wereacquired during two secondary eclipses at the NASA Infrared Telescope Facility(IRTF) in September 2003. We used a circular variable filter (1.5-percentbandpass) centered at 3.8 microns to isolate the predicted flux peak of theplanet at this wavelength. Residual telluric absorption and instrumentvariations were removed by offsetting the telescope to nearby bright comparisonstars at a high temporal cadence. Our results give a secondary eclipse depth of0.0013 +/- 0.0011, not yet sufficient precision to detect the eclipse, whoseexpected depth is approximately 0.002 - 0.003. We here elucidate the currentobservational limitations to this technique, and discuss the approach needed toachieve detections of hot Jupiter secondary eclipses at 3.8 microns from theground.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Any homogeneous polynomial $P(x, y, z)$ of degree $d$, being restricted to aunit sphere $S^2$, admits essentially a unique representation of the form$\\lambda + \\sum_{k = 1}^d [\\prod_{j = 1}^k L_{kj}]$, where $L_{kj}$'s arelinear forms in $x, y$ and $z$ and $\\lambda$ is a real number. The coefficientsof these linear forms, viewed as 3D vectors, are called \\emph{multipole}vectors of $P$. In this paper we consider similar multipole representations ofpolynomial and analytic functions on other quadratic surfaces $Q(x, y, z) = c$,real and complex. Over the complex numbers, the above representation is notunique, although the ambiguity is essentially finite. We investigate thecombinatorics that depicts this ambiguity. We link these results with someclassical theorems of harmonic analysis, theorems that describe decompositionsof functions into sums of spherical harmonics. We extend these classicaltheorems (which rely on our understanding of the Laplace operator$\\Delta_{S^2}$) to more general differential operators $\\Delta_Q$ that areconstructed with the help of the quadratic form $Q(x, y, z)$. Then we introducemodular spaces of multipoles. We study their intricate geometry and topologyusing methods of algebraic geometry and singularity theory. The multipolespaces are ramified over vector or projective spaces, and the compliments tothe ramification sets give rise to a rich family of $K(\\pi, 1)$-spaces, where$\\pi$ runs over a variety of modified braid groups.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "When two-photon interactions are induced by down-converted light with abandwidth that exceeds the pump bandwidth, they can obtain a behavior that ispulse-like temporally, yet spectrally narrow. At low photon fluxes thisbehavior reflects the time and energy entanglement between the down-convertedphotons. However, two-photon interactions such as two-photon absorption (TPA)and sum-frequency generation (SFG) can exhibit such a behavior even at highpower levels, as long as the final state (i.e. the atomic level in TPA, or thegenerated light in SFG) is narrowband enough. This behavior does not depend onthe squeezing properties of the light, is insensitive to linear losses, and haspotential applications. In this paper we describe analytically this behaviorfor travelling-wave down-conversion with continuous or pulsed pumping, both forhigh- and low-power regimes. For this we derive a quantum-mechanical expressionfor the down-converted amplitude generated by an arbitrary pump, and formulateoperators that represent various two-photon interactions induced by broadbandlight. This model is in excellent agreement with experimental results of TPAand SFG with high power down-converted light and with entangled photons [Dayanet al., Phys. Rev. Lett. 93, 023005 (2004), Dayan et al., Phys. Rev. Lett. 94,043602, (2005), Pe'er et al., Phys. Rev. Lett. 94, 073601 (2005)].", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Following an approach based on generating function method phase spacecharacteristics of Landau system are studied in the autonomous framework ofdeformation quantization. Coherent state property of generating functions isestablished and marginal probability densities along canonical coordinate linesare derived. Well defined analogs of inner product, Cauchy-Bunyakowsy-Schwarzinequality and state functional have been defined in phase space and they havebeen used in analyzing the uncertainty structures. The general form of theuncertainty relation for two real-valued functions is derived and uncertaintyproducts are computed in states described by Wigner functions. Minimumuncertainty state property of the standard coherent states is presented anduncertainty structures in the case of phase space generalized coherent statesare analyzed.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We give a quantitative analysis of the previously published nuclear magneticresonance (NMR) experiments in the k-(ET)2X family of organic charge transfersalts by using the phenomenological spin fluctuation model of Moriya, andMillis, Monien and Pines (M-MMP). For temperatures above T_nmr ~ 50 K, themodel gives a good quantitative description of the data in the metallic phasesof several k-(ET)2X materials. These materials display antiferromagneticcorrelation lengths which increase with decreasing temperature and grow toseveral lattice constants by T_nmr. It is shown that the fact that thedimensionless Korringa ratio is much larger than unity is inconsistent with abroad class of theoretical models (such as dynamical mean-field theory) whichneglects spatial correlations and/or vertex corrections. For materials close tothe Mott insulating phase the nuclear spin relaxation rate, the Knight shiftand the Korringa ratio all decrease significantly with decreasing temperaturebelow T_nmr. This cannot be described by the M-MMP model and the most naturalexplanation is that a pseudogap, similar to that observed in the underdopedcuprate superconductors, opens up in the density of states below T_nmr. Such apseudogap has recently been predicted to occur in the dimerised organic chargetransfer salts materials by the resonating valence bond (RVB) theory. Wepropose specific new experiments on organic superconductors to elucidate theseissues. For example, measurements to see if high magnetic fields or highpressures can be used to close the pseudogap would be extremely valuable.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The orbits of stars close to a massive black hole are nearly Keplerianellipses. Such orbits exert long term torques on each other, which lead to anenhanced angular momentum relaxation known as resonant relaxation. Undercertain conditions, this process can modify the angular momentum distributionand affect the interaction rates of the stars with the massive black hole moreefficiently than non-resonant relaxation. The torque on an orbit exerted by thecluster depends on the eccentricity of the orbit. In this paper, we calculatethis dependence and determine the resonant relaxation timescale as a functionof eccentricity. In particular, we show that the component of the torque thatchanges the magnitude of the angular momentum is linearly proportional toeccentricity, so resonant relaxation is much more efficient on eccentric orbitsthan on circular orbits.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We study various topological invariants on a torsional geometry in thepresence of a totally anti-symmetric torsion H under the closed condition dH =0, which appears in string theory compactification scenarios. By using theidentification between the Clifford algebra on the geometry and the canonicalquantization condition of fermions in quantum mechanics, we construct N=1quantum mechanical sigma model in the Hamiltonian formalism. We extend thismodel to N=2 system, equipped with the totally anti-symmetric tensor associatedwith the torsion on the target space geometry. Next we construct transitionelements in the Lagrangian path integral formalism and apply them to theanalyses of the Witten indices in supersymmetric systems. We explicitly showthe formulation of the Dirac index on the torsional manifold which has alreadybeen studied. We also formulate the Euler characteristic and the Hirzebruchsignature on the torsional manifold.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We report on the frequency performance of a low cost (~500$) radio-frequencysine wave generator, using direct digital synthesis (DDS) and afield-programmable gate array (FPGA). The output frequency of the device may bechanged dynamically to any arbitrary value ranging from DC to 10 MHz withoutany phase slip. Sampling effects are substantially reduced by a high samplerate, up to 1 MHz, and by a large memory length, more than 2.10^5 samples. Byusing a low noise external oscillator to clock the DDS, we demonstrate a phasenoise as low as that of the master clock, that is at the level of -113dB.rad^2/Hz at 1 Hz from the carrier for an output frequency of 3.75 MHz. Thedevice is successfully used to confine an ultracold atomic cloud of rubidium 87in a RF-based trap, and there is no extra heating from the RF source.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "In this study, using the analytical and recurrence relations suggested by theauthors in previous works, the new efficient and reliable program procedure forthe overlap integrals over Slater type orbitals (STOs) is presented. Theproposed procedure guarantees a highly accurate evaluation of the overlapintegrals with arbitrary values of quantum numbers, screening constants andinternuclear distances. It is demonstrated that the computational accuracy ofthe proposed procedure is not only dependent on the efficiency of formulas, ashas been discussed previously, but also on a number of other factors includingthe used program language package and solvent properties. The numerical resultsobtained using the algorithm described in the present work are in a completeagreement with those obtained using the alternative evaluation procedure. Wenotice that the program works without any restrictions and in all range ofintegral parameters.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "A consistent device model to describe current-voltage characteristics ofmetal/insulator/metal systems is developed. In this model the insulator and themetal electrodes are described within the same theoretical framework by usingdensity of states distributions. This approach leads to differential equationsfor the electric field which have to be solved in a self consistent manner byconsidering the continuity of the electric displacement and the electrochemicalpotential in the complete system. The model is capable of describing thecurrent-voltage characteristics of the metal/insulator/metal system in forwardand reverse bias for arbitrary values of the metal/ insulator injectionbarriers. In the case of high injection barriers, approximations are providedoffering a tool for comparison with experiments. Numerical calculations areperformed exemplary using a simplified model of an organic semiconductor.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The effect of Li substitution for Mg and of Li-C co-substitution on thesuperconducting properties and crystal structure of MgB2 single crystals hasbeen investigated. It has been found that hole doping with Li decreases thesuperconducting transition temperature Tc, but at a slower rate than electrondoping with C or Al. Tc of MgB2 crystals with simultaneously substituted Li forMg and C for B decreases more than in the case where C is substituted alone.This means that holes introduced by Li cannot counterbalance the effect ofdecrease of Tc caused by introduction of electrons coming from C. The possiblereason of it can be that holes coming from Li occupy the pi band whileelectrons coming from C fill the sigma band. The temperature dependences of theupper critical field Hc2 for Al and Li substituted crystals with the same Tcshow a similar dHc2/dT slope at Tc and a similar Hc2(T) behavior, despite ofmuch different substitution level. This indicates that the mechanismcontrolling Hc2 and Tc is similar in both hole and electron doped crystals.Electrical transport measurements show an increase of resistivity both in Lisubstituted crystals and in Li and C co-substituted crystals. This indicatesenhanced scattering due to defects introduced by substitutions includingdistortion of the lattice. The observed behavior can be explained as a resultof two effects, influencing both Tc and Hc2. The first one is doping related tothe changes in the carrier concentration, which may lead to the decrease or tothe increase of Tc. The second one is related to the introduction of newscattering centers leading to the modification of the interband and/orintraband scattering and therefore, to changes in the superconducting gaps andto the reduction of Tc.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The threshold electrodisintegration of the deuteron at backward angles isstudied with a relativistic Hamiltonian, including a relativisticone-pion-exchange potential (OPEP) with off-shell terms as predicted bypseudovector coupling of pions to nucleons. The bound and scattering states areobtained in the center-of-mass frame, and then boosted from it to the Breitframe, where the evaluation of the relevant matrix elements of theelectromagnetic current operator is carried out. The latter includes, inaddition to one-body, also two-body terms due to pion exchange, as obtained,consistently with the OPEP, in pseudovector pion-nucleon coupling theory. Thefull Lorentz structure of these currents is retained. In order to estimate themagnitude of the relativistic effects we perform, for comparison, thecalculation with a non-relativistic phase-equivalent Hamiltonian and thestandard non-relativistic expressions for the one-body and two-bodypion-exchange currents. Our results for the electrodisintegration cross sectionshow that, in the calculations using one-body currents, relativisticcorrections become significant ({\\it i.e.}, larger than 10%) only at highmomentum transfer $Q$ ($Q^2 \\simeq 40$fm$^{-2}$ and beyond). However, theinclusion of two-body currents makes the relativistic predictions considerablysmaller than the corresponding non-relativistic results in the $Q^2$ region(18--40) fm$^{-2}$. The calculations based on the relativistic model alsoconfirm the inadequacy, already established in a non-relativistic context, ofthe present electromagnetic current model to reproduce accurately theexperimental data at intermediate values of momentum transfers.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Building on the well-known Unruh-Davies effect, we examine the effects ofprojective measurements and quantum communications between accelerated andstationary observers. We find that the projective measurement by a uniformlyaccelerated observer can excite real particles from the vacuum in the inertialframe, even if no additional particles are created by the measurement processin the accelerating frame. Furthermore, we show that the particles created bythis accelerating measurement can be highly entangled in the inertial frame,and it is also possible to use this process to generate even maximallyentangled two-qubit states by a certain arrangement of measurements. As abyproduct of our analysis, we also show that a single qubit of information canbe perfectly transmitted from the accelerating observer to the inertial one. Inprinciple, such an effect could be exploited in designing an entangled stategenerator for quantum communication.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "In the work of Hoshino, Kato and Miyachi, the authors look at t-structuresinduced by a compact object, C, of a triangulated category, T, which is rigidin the sense of Iyama and Yoshino. Hoshino, Kato and Miyachi show that such anobject yields a non-degenerate t-structure on T whose heart es equivalent toMod(End(C)^op). Rigid objects in a triangulated category can be thought of asbehaving like chain differential graded algebras (DGAs).  Analogously, looking at objects which behave like cochain DGAs naturallygives the dual notion of a corigid object. Here, we see that a compact corigidobject, S, of a triangulated category, T, induces a structure similar to at-structure which we shall call a co-t-structure. We also show that the coheartof this non-degenerate co-t-structure is equivalent to Mod(End(S)^op), andhence an abelian subcategory of T.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We argue that non-Abelian gauge fields can be treated as the pseudo-Goldstonevector bosons caused by spontaneous Lorentz invariance violation (SLIV). Tothis end, the SLIV which evolves in a general Yang-Mills type theory with thenonlinear vector field constraint $Tr(% \\boldsymbol{A}_{\\mu}\\boldsymbol{A}^{\\mu})=\\pm M^{2}$ ($M$ is a proposed SLIV scale) imposed isconsidered in detail. With an internal symmetry group $G$ having $D$ generatorsnot only the pure Lorentz symmetry SO(1,3), but the larger accidental symmetry$SO(D,3D)$ of the SLIV constraint in itself appears to be spontaneously brokenas well. As a result, while the pure Lorentz violation still generates only onegenuine Goldstone vector boson, the accompanying pseudo-Goldstone vector bosonsrelated to the $SO(D,3D)$ breaking also come into play in the final arrangementof the entire Goldstone vector field multiplet. Remarkably, they remainstrictly massless, being protected by gauge invariance of the Yang-Mills theoryinvolved. We show that, although this theory contains a plethora of Lorentz and$CPT$ violating couplings, they do not lead to physical SLIV effects which turnout to be strictly cancelled in all the lowest order processes considered.However, the physical Lorentz violation could appear if the internal gaugeinvariance were slightly broken at very small distances influenced by gravity.For the SLIV scale comparable with the Planck one the Lorentz violation couldbecome directly observable at low energies.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Near-IR and X-ray flares have been detected from the supermassive black holeSgr A* at the center of our Galaxy with a (quasi)-period of ~17-20 minutes,suggesting an emission region only a few Schwarzschild radii above the eventhorizon. The latest X-ray flare, detected with XMM-Newton, is notable for itsdetailed lightcurve, yielding not only the highest quality period thus far, butalso important structure reflecting the geometry of the emitting region. RecentMHD simulations of Sgr A*'s disk have demonstrated the growth of a Rossby waveinstability, that enhances the accretion rate for several hours, possiblyaccounting for the observed flares. In this Letter, we carry out ray-tracingcalculations in a Schwarzschild metric to determine as accurately as possiblethe lightcurve produced by general relativistic effects during such adisruption. We find that the Rossby wave induced spiral pattern in the disk isan excellent fit to the data, implying a disk inclination angle of ~77 deg.Note, however, that if this association is correct, the observed period is notdue to the underlying Keplerian motion but, rather, to the pattern speed. Thefavorable comparison between the observed and simulated lightcurves providesimportant additional evidence that the flares are produced in Sgr A*'s innerdisk.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "In the classical one-dimensional solution of fluid dynamics equations allunknown functions depend only on time t and Cartesian coordinate x. Althoughfluid spreads in all directions (velocity vector has three components) thewhole picture of motion is relatively simple: trajectory of one fluid particlefrom plane x=const completely determines motion of the whole plane. Basing onthe symmetry analysis of differential equations we propose generalization ofthis solution allowing movements in different directions of fluid particlesbelonging to plane x=const. At that, all functions but an angle determining thedirection of particle's motion depend on t and x only, whereas the angledepends on all coordinates. In this solution the whole picture of motionsuperposes from identical trajectories placed under different angles in 3Dspace. Orientations of the trajectories are restricted by a finite relationpossessing functional arbitrariness. The solution describes three-dimensionalnonlinear processes and singularities in infinitely conducting plasma, gas orincompressible liquid.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The function exp(iwt) describes an oscillating motion. Energy of theoscillator is proportional to the square of w. exp(iwt) is the solution of adifferential equation. We have replaced this differential equation by thecorresponding finite-time difference equation with d as the smallest span oftime. We have, then, symmetrized the equation so that it remains invariantunder the change d going to -d. This symmetric equation has solutions in pairs.The angular speed w is modified to w' or w\". w' contains a part with aninteger. w\" contains a part with a half-integer. This corresponds to quantummechanical oscillator energy levels. F= a.exp(iwt) describes oscillationbetween -a and +a. If we make w=0, F describes free oscillation between -a and+a. Reciprocal symmetric oscillator, thus, unifies quantum and classicalharmonic oscillators on one hand, and a harmonic oscillator and a free particlein a potential well on the other hand. No quantum mechanical postulates areinvolved.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present new observational results obtained for the Galactic non-thermalradio source G328.4+0.2 to determine both if this source is a pulsar windnebula or supernova remnant, and in either case, the physical properties ofthis source. Using X-ray data obtained by XMM, we confirm that the X-rayemission from this source is heavily absorbed and has a spectrum best fit by apower law model of photon index=2 with no evidence for a thermal component, theX-ray emission from G328.4+0.2 comes from a region significantly smaller thanthe radio emission, and that the X-ray and radio emission are significantlyoffset from each other. We also present the results of a new high resolution (7arcseconds) 1.4 GHz image of G328.4+0.2 obtained using the Australia TelescopeCompact Array, and a deep search for radio pulsations using the Parkes RadioTelescope. We find that the radio emission has a flat spectrum, though someareas along the eastern edge of G328.4+0.2 have a steeper radio spectral indexof ~-0.3. Additionally, we obtain a luminosity limit of the central pulsar ofL_{1400} < 30 mJy kpc^2, assuming a distance of 17 kpc. In light of theseobservational results, we test if G328.4+0.2 is a pulsar wind nebula (PWN) or alarge PWN inside a supernova remnant (SNR) using a simple hydrodynamic modelfor the evolution of a PWN inside a SNR. As a result of this analysis, weconclude that G328.4+0.2 is a young (< 10000 years old) pulsar wind nebulaformed by a low magnetic field (<10^12 G) neutron star born spinning rapidly(<10 ms) expanding into an undetected SNR formed by an energetic (>10^51 ergs),low ejecta mass (M < 5 Solar Masses) supernova explosion which occurred in alow density (n~0.03 cm^{-3}) environment.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The effect of possible in-medium modifications of nucleon-nucleon ($NN$)cross sections on particle production is investigated in heavy ion collisions($HIC$) at intermediate energies. In particular, using a fully covariantrelativistic transport approach, we see that the density dependence of the {\\itinelastic} cross sections appreciably affects the pion and kaon yields andtheir rapidity distributions. However, the $(\\pi^{-}/\\pi^{+})$- and$(K^{0}/K^{+})$-ratios depend only moderately on the in-medium behavior of theinelastic cross sections. This is particularly true for kaon yield ratios,since kaons are more uniformly produced in high density regions. Kaonpotentials are also suitably evaluated in two schemes, a chiral perturbativeapproach and an effective meson-quark coupling method, with consistent resultsshowing a similar repulsive contribution for $K^{+}$ and $K^{0}$. As aconsequence we expect rather reduced effects on the yield ratios. We concludethat particle ratios appear to be robust observables for probing the nuclearequation of state ($EoS$) at high baryon density and, particularly, itsisovector sector.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The early-R stars are carbon-rich K-type giants. They are enhanced in C12,C13 and N14, have approximately solar oxygen, magnesium isotopes, s-process andiron abundances, have the luminosity of core-helium burning stars, are notrapid rotators, are members of the Galactic thick disk and, most peculiarly ofall, are all single stars. Conventional single-star stellar evolutionary modelscannot explain such stars, but mergers in binary systems have been proposed toexplain their origin.  We have synthesized binary star populations to calculate the number of mergedstars with helium cores which could be early-R stars. We find many possibleevolutionary channels. The most common of which is the merger of a helium whitedwarf with a hydrogen-burning red giant branch star during a common envelopephase followed by a helium flash in a rotating core which mixes carbon to thesurface. All the channels together give ten times more early-R stars than werequire to match recent Hipparcos observations - we discuss which channels arelikely to be the true early-R stars and which are not. For the first time wehave constructed a viable model of the early-R stars with which we can testsome of our ideas regarding common envelope evolution in giants, stellarmergers, rotation, the helium flash and the origin of the early-R stars.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "After the nontrivial quantum parameters $\\Omega_{n}$ and quantum potentials$V_{n}$ obtained in our previous research, the circumstance of a real scalarwave in the bulk is studied with the similar method of Brevik (2001). Theequation of a massless scalar field is solved numerically under the boundaryconditions near the inner horizon $r_{e}$ and the outer horizon $r_{c}$. Unlikethe usual wave function $\\Psi_{\\omega l}$ in 4D, quantum number $n$ introducesa new functions $\\Psi_{\\omega l n}$, whose potentials are higher and wider withbigger n. Using the tangent approximation, a full boundary value problem aboutthe Schr$\\ddot{o}$dinger-like equation is solved. With a convenient replacementof the 5D continuous potential by square barrier, the reflection andtransmission coefficients are obtained. If extra dimension does exist and isvisible at the neighborhood of black holes, the unique wave function$\\Psi_{\\omega l n}$ may say something to it.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "CO observations have been so far the best way to trace molecular gas inexternal galaxies, but at low metallicity the gas mass deduced could be largelyunderestimated. At present, the kinematic information of CO data cubes are usedto estimate virial masses and trace the total mass of the molecular clouds.Millimeter dust emission can also be used as a dense gas tracer and couldunveil H2 envelopes lacking CO. These different tracers must be compared indifferent environments. This study compares virial masses to masses deducedfrom millimeter emission, in two GMC samples: the local molecular clouds in ourGalaxy and their equivalents in the Small Magellanic Cloud (SMC), one of thenearest low metallicity dwarf galaxy. In our Galaxy, mass estimates deducedfrom millimeter emission are consistent with masses deduced from gamma rayanalysis and trace the total mass of the clouds. Virial masses aresystematically larger (twice on average) than mass estimates from millimeterdust emission. This difference decreases toward high masses and has alreadybeen reported in previous studies. In the SMC however, molecular cloud massesdeduced from SIMBA millimeter observations are systematically higher (twice onaverage for conservative values of the dust to gas ratio and dust emissivity)than the virial masses from SEST CO observations. The observed excess can notbe accounted for by any plausible change of dust properties. Taking a generalform for the virial theorem, we show that a magnetic field strength of ~15micro Gauss in SMC clouds could provide additional support to the clouds andexplain the difference observed. Masses of SMC molecular clouds have thereforebeen underestimated so far. Magnetic pressure may contribute significantly totheir support.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The Gauss map of non-degenerate surfaces in the three-dimensional Minkowskispace are viewed as dynamical fields of the two-dimensional O(2,1) NonlinearSigma Model. In this setting, the moduli space of solutions with rotationalsymmetry is completely determined. Essentially, the solutions are warpedproducts of orbits of the 1-dimensional groups of isometries and elastic curvesin either a de Sitter plane, a hyperbolic plane or an anti de Sitter plane. Themain tools are the equivalence of the two-dimensional O(2,1) Nonlinear SigmaModel and the Willmore problem, and the description of the surfaces withrotational symmetry. A complete classification of such surfaces is obtained inthis paper. Indeed, a huge new family of Lorentzian rotational surfaces with aspace-like axis is presented. The description of this new class of surfaces isbased on a technique of surgery and a gluing process, which is illustrated byan algorithm.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We report on measurements of the adiabatic temperature change in the inversemagnetocaloric Ni$_{50}$Mn$_{34}$In$_{16}$ alloy. It is shown that this alloyheats up with the application of a magnetic field around the Curie point due tothe conventional magnetocaloric effect. In contrast, the inverse magnetocaloriceffect associated with the martensitic transition results in the unusualdecrease of temperature by adiabatic magnetization. We also providemagnetization and specific heat data which enable to compare the measuredtemperature changes to the values indirectly computed from thermodynamicrelationships. Good agreement is obtained for the conventional effect at thesecond-order paramagnetic-ferromagnetic phase transition. However, at the firstorder structural transition the measured values at high fields are lower thanthe computed ones. Irreversible thermodynamics arguments are given to show thatsuch a discrepancy is due to the irreversibility of the first-order martensitictransition.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "In the absence of direct kinematic measurements, the mass of an accretingblack hole is sometimes inferred from the X-ray spectral parameters of itsaccretion disk; specifically, from the temperature and normalization of adisk-blackbody model fit. Suitable corrections have to be introduced when theaccretion rate approaches or exceeds the Eddington limit. We summarizephenomenological models that can explain the very high state, with apparentlyhigher disk temperatures and lower inner-disk radii. Conversely, ultraluminousX-ray sources often contain cooler disks with large characteristic radii. Weintroduce another phenomenological model for this accretion state. We arguethat a standard disk dominates the radiative output for radii larger than acharacteristic transition radius R_c ~ mdot x R_{ISCO}, where mdot is theaccretion rate in Eddington units and R_{ISCO} is the innermost stable orbit.For R_{ISCO} < R < R_c, most of the accretion power is released via non-thermalprocesses. We predict the location of such sources in a luminosity-temperatureplot. We conclude that black holes with masses ~ 50-100 Msun accreting at mdot~ 10-20 may explain the X-ray properties of many ULXs.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We study phonon-mediated transitions between translational levels of an atomin a surface-induced potential. We present a general master equation governingthe dynamics of the translational states of the atom. In the framework of theDebye model, we derive compact expressions for the rates for both upward anddownward transitions. Numerical calculations for the transition rates areperformed for a deep silica-induced potential allowing for a large number ofbound levels as well as free states of a cesium atom. The total absorption rateis shown to be determined mainly by the bound-to-bound transitions for deepbound levels and by bound-to-free transitions for shallow bound levels.Moreover, the phonon emission and absorption processes can be orders ofmagnitude larger for deep bound levels as compared to the shallow bound ones.We also study various types of transitions from free states. We show that, forthermal atomic cesium with temperature in the range from 100 $\\mu$K to 400$\\mu$K in the vicinity of a silica surface with temperature of 300 K, theadsorption (free-to-bound decay) rate is about two times larger than theheating (free-to-free upward decay) rate, while the cooling (free-to-freedownward decay) rate is negligible.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We consider a cognitive network consisting of n random pairs of cognitivetransmitters and receivers communicating simultaneously in the presence ofmultiple primary users. Of interest is how the maximum throughput achieved bythe cognitive users scales with n. Furthermore, how far these users must befrom a primary user to guarantee a given primary outage. Two scenarios areconsidered for the network scaling law: (i) when each cognitive transmitteruses constant power to communicate with a cognitive receiver at a boundeddistance away, and (ii) when each cognitive transmitter scales its poweraccording to the distance to a considered primary user, allowing the cognitivetransmitter-receiver distances to grow. Using single-hop transmission, suitablefor cognitive devices of opportunistic nature, we show that, in both scenarios,with path loss larger than 2, the cognitive network throughput scales linearlywith the number of cognitive users. We then explore the radius of a primaryexclusive region void of cognitive transmitters. We obtain bounds on thisradius for a given primary outage constraint. These bounds can help in thedesign of a primary network with exclusive regions, outside of which cognitiveusers may transmit freely. Our results show that opportunistic secondaryspectrum access using single-hop transmission is promising.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We consider the simplest generalizations of the valence bond physics of SU(2)singlets to SU(N) singlets that comprise objects with N sites -- these areSU(N) singlet plaquettes with N=3 and N=4 in three spatial dimensions.Specifically, we search for a quantum mechanical liquid of such objects -- aresonating singlet valence plaquette phase that generalizes the celebratedresonating valence bond phase for SU(2) spins. We extend the Rokhsar-Kivelsonconstruction of the quantum dimer model to the simplest SU(4) model for valenceplaquette dynamics on a cubic lattice. The phase diagram of the resultingquantum plaquette model is analyzed both analytically and numerically. We findthat the ground state is solid everywhere, including at the Rokhsar-Kivelsonpoint where the ground state is an equal amplitude sum. By contrast, the equalamplitude sum of SU(3) singlet triangular plaquettes on the face centered cubiclattice is liquid and thus a candidate for describing a resonating singlevalence plaquette phase, given a suitably defined local Hamiltonian.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "From several points of view it is strongly suggested that the currentuniverse is unstable and will ultimately decay to one that is exactlysupersymmetric (susy). The possibility that atoms and molecules form in thisfuture universe requires that the degenerate electron/selectron mass isnon-zero and hence that electroweak symmetry breaking (EWSB) survives the phasetransition to exact susy. However, the minimal supersymmetric standard model(MSSM) and several of its extensions have no EWSB in the susy limit. Among theextended higgs models that have been discussed one stands out in this regard.The higgs sector that is revealed at the Large Hadron Collider (LHC) willtherefore have implications for the future universe. We also address thequestion as to whether the transition to the exact susy phase with EWSB isexothermic.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present observations of probable line-of-sight acceleration of a broadabsorption trough of C IV in the quasar SDSS J024221.87+004912.6. We alsodiscuss how the velocity overlap of two other outflowing systems in the sameobject constrains the properties of the outflows. The Si IV doublet in eachsystem has one unblended transition and one transition which overlaps withabsorption from the other system. The residual flux in the overlapping troughis well fit by the product of the residual fluxes in the unblended troughs. Forthese optically thick systems to yield such a result, at least one of them mustconsist of individual subunits rather than being a single structure withvelocity-dependent coverage of the source. If these subunits are identical,opaque, spherical clouds, we estimate the cloud radius to be r = 3.9 10^15 cm.If they are identical, opaque, linear filaments, we estimate their width to bew = 6.5 10^14 cm. These subunits are observed to cover the Mg II broad emissionline region of the quasar, at which distance from the black hole the abovefilament width is equal to the predicted scale height of the outer atmosphereof a thin accretion disk. Insofar as that scale height is a natural size scalefor structures originating in an accretion disk, these observations areevidence that the accretion disk can be a source of quasar absorption systems.Based on data from ESO program 075.B-0190(A).", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Atmospheric water vapor causes significant undesired phase fluctuations forthe Submillimeter Array (SMA) interferometer, particularly in its highestfrequency observing band of 690 GHz. One proposed solution to this atmosphericeffect is to observe simultaneously at two separate frequency bands of 230 and690 GHz. Although the phase fluctuations have a smaller magnitude at the lowerfrequency, they can be measured more accurately and on shorter timescales dueto the greater sensitivity of the array to celestial point source calibratorsat this frequency. In theory, we can measure the atmospheric phase fluctuationsin the 230 GHz band, scale them appropriately with frequency, and apply them tothe data in 690 band during the post-observation calibration process. Theultimate limit to this atmospheric phase calibration scheme will be set by theinstrumental phase stability of the IF and LO systems. We describe themethodology and initial results of the phase stability characterization of theIF and LO systems.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Multiwavelength observations are reported here of the Be/X-ray binary pulsarsystem GRO J1008-57. Over ten years worth of data are gathered together to showthat the periodic X-ray outbursts are dependant on both the binary motion andthe size of the circumstellar disk. In the first instance an accurate orbitalsolution is determined from pulse periods, and in the second case the strengthand shape of the Halpha emission line is shown to be a valuable indicator ofdisk size and its behaviour. Furthermore, the shape of the emission linepermits a direct determination of the disk size which is in good agreement withtheoretical estimates. A detailed study of the pulse period variations duringoutbursts determined the binary period to be 247.8, in good agreement with theperiod determined from the recurrence of the outbursts.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We investigate theoretically and experimentally the capillary-gravity wavescreated by a small object moving steadily at the water-air interface along acircular trajectory. It is well established that, for straight uniform motion,no steady waves appear at velocities below the minimum phase velocity $c_{min}= 23 \\rm{cm \\cdot s}^{-1}$. We show theoretically that no such velocitythreshold exists for a steady circular motion, for which, even at smallvelocities, a finite wave drag is experienced by the object. This wave dragoriginates from the emission of a spiral-like wave pattern. Our results are ingood agreement with direct experimental observations of the wave patterncreated by a circularly moving needle in contact with water. Our study leads tonew insights into the problem of animal locomotion at the water-air interface.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We develop here a mechanism that, without making use of a cosmologicalconstant, reproduces an accelerating universe. This is done by taking intoaccount Casimir vacuum energy density, assuming that the underlying theoryallows a maximum momentum, that turns out to be the leading contribution termto Einstein equations in a large expanding FRW universe. As stated in numerousquantum gravity studies, we postulate that maximum momentum is related to theexistence of the Planck length as a fundamental length. This insight, togetherwith the assumption of a Planck scale correction to the energy/momentumdispersion-relation on a FRW background, is used here to calculate Casimirvacuum energy. We show that, under these hypothesis, an accelerated universeexpansion is obtained. As last step we analyze the compatibility of theresulting model with experimental data, writing down the equation of state forCasimir energy and pressure and observing that this equation of state belongsto a class of models that naturally fits cosmological observations. Weemphasize that our result relies, once a fundamental length is introduced inCasimir effect, just on general arguments thus it is independent on an explicitform of the energy-momentum dispersion relation.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Our group recently reproduced the water-assisted growth method, so-called\"super growth\", of millimeter-thick single-walled carbon nanotube (SWNT)forests by using C2H4/ H2/ H2O/ Ar reactant gas and Fe/ Al2O3 catalyst. In thiscurrent work, a parametric study was carried out on both reaction and catalystconditions. Results revealed that a thin Fe catalyst layer (about 0.5 nm)yielded rapid growth of SWNTs only when supported on Al2O3, and that Al2O3support enhanced the activity of Fe, Co, and Ni catalysts. The growth windowfor the rapid SWNT growth was narrow, however. Optimum amount of added H2Oincreased the SWNT growth rate but further addition of H2O degraded both theSWNT growth rate and quality. Addition of H2 was also essential for rapid SWNTgrowth, but again, further addition decreased both the SWNT growth rate andquality. Because Al2O3 catalyzes hydrocarbon reforming, Al2O3 support possiblyenhances the SWNT growth rate by supplying the carbon source to the catalystnanoparticles. The origin of the narrow window for rapid SWNT growth will alsobe discussed.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "This paper proposes the use of particle swarm optimization method (PSO) forfinite element (FE) model updating. The PSO method is compared to the existingmethods that use simulated annealing (SA) or genetic algorithms (GA) for FEmodel for model updating. The proposed method is tested on an unsymmetricalH-shaped structure. It is observed that the proposed method gives updatednatural frequencies the most accurate and followed by those given by an updatedmodel that was obtained using the GA and a full FE model. It is also observedthat the proposed method gives updated mode shapes that are best correlated tothe measured ones, followed by those given by an updated model that wasobtained using the SA and a full FE model. Furthermore, it is observed that thePSO achieves this accuracy at a computational speed that is faster than that bythe GA and a full FE model which is faster than the SA and a full FE model.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We investigate whether the floating phase (where the correlation length isinfinite and the spin-spin correlation decays algebraically with distance)exists in the temperature($T$) - frustration parameter ($\\kappa$) phase diagramof 2D ANNNI model. To identify this phase, we look for the region where (i)finite size effect is prominent and (ii) some relevant physical quantitychanges somewhat sharply and this change becomes sharper as the system sizeincreases. For $\\kappa < 0.5 $, the low temperature phase is ferromagnetic andwe study energy and magnetization. For $\\kappa > 0.5 $, the low temperaturephase is antiphase and we study energy, layer magnetization, length of domainwalls running along the direction of frustration, number of domain-interceptsthat are of length 2 along the direction of frustration, and the number ofdomain walls that do not touch the upper and/or lower boundary. In agreementwith some previous studies, our final conclusion is that, the floating phaseexists, if at all, only along a line.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We study the effects of lepton flavour violation (LFV) on the productionprocesses e+e- --> \\chi+_i \\chi-_j at a linear collider with longitudinal e+and e- beam polarizations. In the case of LFV the sneutrino mass eigenstateshave no definite flavour, therefore, in the t-channel more than one sneutrinomass eigenstate can contribute to the chargino production cross sections. Ourframework is the Minimal Supersymmetric Standard Model (MSSM) including LFVterms. We show that in spite of the restrictions on the LFV parameters due tothe current limits on rare lepton decays, the cross section \\sigma(e+e- -->\\chi+_1 \\chi-_1) can change by a factor of 2 or more when varying the LFVmixing angles. We point out that even if the present bound on BR(tau- --> e-gamma) improves by a factor of thousand the influence of LFV on the charginoproduction cross section can be significant. These results could have animportant impact on the strategies for determining the underlying modelparameters at the linear collider.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We employ X-ray stacking techniques to examine the contribution from X-rayundetected, mid-infrared-selected sources to the unresolved, hard (6-8 keV)cosmic X-ray background (CXB). We use the publicly available, 24 micron SpitzerSpace Telescope MIPS catalogs from the Great Observatories Origins Deep Survey(GOODS) - North and South fields, which are centered on the 2 Ms Chandra DeepField-North and the 1 Ms Chandra Deep Field-South, to identify bright (S_24 >80 microJy) mid-infrared sources that may be powered by heavily obscured AGNs.We measure a significant stacked X-ray signal in all of the X-ray bandsexamined, including, for the first time, a significant (3.2 sigma) 6-8 keVstacked X-ray signal from an X-ray undetected source population. We find thatthe X-ray-undetected MIPS sources make up about 2% (or less) of the total CXBbelow 6 keV, but about 6% in the 6-8 keV band. The 0.5-8 keV stacked X-rayspectrum is consistent with a hard power-law (Gamma = 1.44 +/- 0.07), with thespectrum hardening at higher X-ray energies. Our findings show that thesebright MIPS sources do contain obscured AGNs, but are not the primary source ofthe unresolved 50% of 6-8 keV CXB. Our study rules out obscured, luminous QSOsas a significant source of the remaining unresolved CXB and suggests that itmost likely arises from a large population of obscured, high-redshift (z > 1),Seyfert-luminosity AGNs.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Formal actions of Lie algebras over vector spaces are introduced in a purelyalgebraic way, as a mimic of infinitesimal operations of Banach Lie algebrasover Banach analytic manifolds. In analogy with the case of abstract groups,complete wreath products and triangular actions are then defined for Liealgebras acting \"en cascade\" over vector spaces. Finally, a Kaloujnine-Krasnertype theorem for Lie algebra extensions is proved.  -----  En mimant les lois d'op\\'erations infinit\\'esimales des alg\\`ebres de Lie surles vari\\'et\\'e s analytiques banachiques, on introduit de mani\\`ere purementalg\\`ebrique la notion d'action formelle d'une alg\\`ebre de Lie sur un espacevectoriel. Ensuite, par analogie avec le cas des groupes abstraits, et enfaisant op\\'erer les alg\\`ebres de Lie \"en cascade\", on d\\'efinit produitd'entrelacement (\"wreath product\") et action triangulaire pour les alg\\`ebresde Lie. On d\\'emontre enfin un th\\'eor\\`eme du type Kaloujnine-Krasner pour lesextensions d'alg\\`ebres de Lie.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "A theory of chiral lipid membranes is proposed on the basis of a concise freeenergy density which includes the contributions of the bending and the surfacetension of membranes, as well as the chirality and orientational variation oftilting molecules. This theory is consistent with the previous experiments[J.M. Schnur \\textit{et al.}, Science \\textbf{264}, 945 (1994); M.S. Spector\\textit{et al.}, Langmuir \\textbf{14}, 3493 (1998); Y. Zhao, \\textit{et al.},Proc. Natl. Acad. Sci. USA \\textbf{102}, 7438 (2005)] on self-assembled chirallipid membranes of DC$_{8,9}$PC. A torus with the ratio between its twogenerated radii larger than $\\sqrt{2}$ is predicted from the Euler-Lagrangeequations. It is found that tubules with helically modulated tilting state arenot admitted by the Euler-Lagrange equations, and that they are lessenergetically favorable than helical ripples in tubules. The pitch angles ofhelical ripples are theoretically estimated to be about 0$^\\circ$ and35$^\\circ$, which are close to the most frequent values 5$^\\circ$ and28$^\\circ$ observed in the experiment [N. Mahajan \\textit{et al.}, Langmuir\\textbf{22}, 1973 (2006)]. Additionally, the present theory can explain twistedribbons of achiral cationic amphiphiles interacting with chiral tartratecounterions. The ratio between the width and pitch of twisted ribbons ispredicted to be proportional to the relative concentration difference of left-and right-handed enantiomers in the low relative concentration differenceregion, which is in good agreement with the experiment [R. Oda \\textit{et al.},Nature (London) \\textbf{399}, 566 (1999)].", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We use high-resolution hydrodynamic re-simulations to investigate theproperties of the thermal Sunyaev-Zel'dovich (SZ) effect from galaxy clusters.We compare results obtained using different physical models for theintracluster medium (ICM), and show how they modify the SZ emission in terms ofcluster profiles and scaling relations. We also produce realistic mockobservations to verify whether the results from hydrodynamic simulations can beconfirmed. We find that SZ profiles depend marginally on the modelled physicalprocesses, while they exhibit a strong dependence on cluster mass. The centraland total SZ emission strongly correlate with the cluster X-ray luminosity andtemperature. The logarithmic slopes of these scaling relations differ from theself-similar predictions by less than 0.2; the normalization of the relationsis lower for simulations including radiative cooling. The observational testsuggests that SZ cluster profiles are unlikely to be able to probe the ICMphysics. The total SZ decrement appears to be an observable much more robustthan the central intensity, and we suggest using the former to investigatescaling relations.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Given a finite irreducible Coxeter group $W$, a positive integer $d$, andtypes $T_1,T_2,...,T_d$ (in the sense of the classification of finite Coxetergroups), we compute the number of decompositions $c=\\si_1\\si_2 cdots\\si_d$ of aCoxeter element $c$ of $W$, such that $\\si_i$ is a Coxeter element in asubgroup of type $T_i$ in $W$, $i=1,2,...,d$, and such that the factorisationis \"minimal\" in the sense that the sum of the ranks of the $T_i$'s,$i=1,2,...,d$, equals the rank of $W$. For the exceptional types, thesedecomposition numbers have been computed by the first author. The type $A_n$decomposition numbers have been computed by Goulden and Jackson, albeit using asomewhat different language. We explain how to extract the type $B_n$decomposition numbers from results of B\\'ona, Bousquet, Labelle and Leroux onmap enumeration. Our formula for the type $D_n$ decomposition numbers is new.These results are then used to determine, for a fixed positive integer $l$ andfixed integers $r_1\\le r_2\\le ...\\le r_l$, the number of multi-chains $\\pi_1\\le\\pi_2\\le ...\\le \\pi_l$ in Armstrong's generalised non-crossing partitionsposet, where the poset rank of $\\pi_i$ equals $r_i$, and where the \"blockstructure\" of $\\pi_1$ is prescribed. We demonstrate that this result impliesall known enumerative results on ordinary and generalised non-crossingpartitions via appropriate summations. Surprisingly, this result on multi-chainenumeration is new even for the original non-crossing partitions of Kreweras.Moreover, the result allows one to solve the problem of rank-selected chainenumeration in the type $D_n$ generalised non-crossing partitions poset, which,in turn, leads to a proof of Armstrong's $F=M$ Conjecture in type $D_n$.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "In this paper a lattice model for diffusional transport of particles in theinterphase cell nucleus is proposed. Dense networks of chromatin fibers arecreated by three different methods: randomly distributed, non-interconnectedobstacles, a random walk chain model, and a self avoiding random walk chainmodel with persistence length. By comparing a discrete and a continuous versionof the random walk chain model, we demonstrate that lattice discretization doesnot alter particle diffusion. The influence of the 3D geometry of the fibernetwork on the particle diffusion is investigated in detail, while varyingoccupation volume, chain length, persistence length and walker size. It isshown that adjacency of the monomers, the excluded volume effect incorporatedin the self avoiding random walk model, and, to a lesser extent, thepersistence length, affect particle diffusion. It is demonstrated how theintroduction of the effective chain occupancy, which is a convolution of thegeometric chain volume with the walker size, eliminates the conformationaleffects of the network on the diffusion, i.e., when plotting the diffusioncoefficient as a function of the effective chain volume, the data fall onto amaster curve.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The damage spreading method (DS) provided a useful tool to obtain analyticalresults of the thermodynamics and stability of the 2D Ising model --amongstmany others--, but it suffered both from ambiguities in its results and fromlarge computational costs. In this paper we propose an alternative method, theso called self-overlap method, based on the study of correlation functionsmeasured at subsequent time steps as the system evolves towards itsequilibrium. Applying markovian and mean field approximations to a 2D Isingsystem we obtain both analytical and numerical results on the thermodynamicsthat agree with the expected behavior. We also provide some analytical resultson the stability of the system. Since only a single replica of the system needsto be studied, this method would seem to be free from the ambiguities thatafflicted DS. It also seems to be numerically more efficient and analyticallysimpler.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The magnetic focusing of electrons has proven its utility in fundamentalstudies of electron transport. Here we report the direct imaging of magneticfocusing of electron waves, specifically in a two-dimensional electron gas(2DEG). We see the semicircular trajectories of electrons as they bounce alonga boundary in the 2DEG, as well as fringes showing the coherent nature of theelectron waves. Imaging flow in open systems is made possible by a cooledscanning probe microscope. Remarkable agreement between experiment and theorydemonstrates our ability to see these trajectories and to use this system as aninterferometer. We image branched electron flow as well as the interference ofelectron waves. This technique can visualize the motion of electron wavesbetween two points in an open system, providing a straightforward way to studysystems that may be useful for quantum information processing and spintronics.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We propose a gravitational dual of ``single-sector'' models of supersymmetrybreaking which contain no messenger sector and naturally explain the scale ofsupersymmetry breaking and the fermion mass hierarchy. In five dimensions thesemodels can be given a simple interpretation. Inspired by flux-backgroundsolutions of type IIB supergravity, a metric background that deviates fromAdS_5 in the IR breaks supersymmetry, while the fermion mass hierarchy resultsfrom the wavefunction overlap of bulk fermions with a UV-confined Higgs field.The first and second generation squarks and sleptons, which are localized nearthe IR brane, directly feel the supersymmetry breaking and obtain masses oforder 10 TeV. These are interpreted as composite states of the dual 4D theory.The gauginos and third generation squarks and sleptons are elementary statesthat obtain soft masses of order 1 TeV at the loop level via direct gaugemediation. This particle spectrum leads to distinctive signatures at the LHC,similar to the usual gauge mediation with a neutralino NLSP that decayspromptly to a gravitino LSP, but with lower event rates. Nevertheless we showthat with 1-10 fb^{-1} of LHC data \"single-sector\" models can easily bedetected above background and distinguished from conventional gravity and gaugemediation.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We investigate the evolution of the electronic structure in SrRu_(1-x)Ti_xO_3as a function of x using high resolution photoemission spectroscopy, whereSrRuO3 is a weakly correlated metal and SrTiO3 is a band insulator. The surfacespectra exhibit a metal-insulator transition at x = 0.5 by opening up a softgap. A hard gap appears at higher x values consistent with the transportproperties. In contrast, the bulk spectra reveal a pseudogap at the Fermilevel, and unusual evolution exhibiting an apparent broadening of the coherentfeature and subsequent decrease in intensity of the lower Hubbard band with theincrease in x. Interestingly, the first principle approaches are found to besufficient to capture anomalous evolutions at high energy scale. Analysis ofthe spectral lineshape indicates strong interplay between disorder and electroncorrelation in the electronic properties of this system.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "In the Randall-Sundrum model, setting the ratio of up and down quark masses$m_u/m_d << 1$, relevant to the strong CP problem, does not require chiralsymmetry or fine-tuning, due to exponential bulk fermion profiles. We point outthat such geometric suppression of the mass of a fermion magnifies the massesof its corresponding Kaluza-Klein (KK) states. In this sense, these KK statesact as \"microscopes\" for probing light quark and lepton masses. In simplerealizations, this hypothesis can be testable at future colliders, like theLHC, by measuring the spectrum of level-1 KK fermions. The microscope can thenprovide an experimental test for the vanishing of $m_u$ in the ultraviolet,independently of non-perturbative determinations, by lattice simulations orother means, at hadronic scales. We also briefly comment on application of ourmicroscope idea to other fermions, such as the electron and neutrinos.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The standard axiomatization of quantum mechanics (QM) is not fully explicitabout the role of the time-parameter. Especially, the time reference within theprobability algorithm (the Born Rule, BR) is unclear. Using a plausibleprinciple P1, about the role of probability in a physical theory, and a secondprinciple P2 affording a most natural way to make BR precise, a logicalconflict with the standard expression for the completeness of QM can bederived. Rejecting P1 is implausible. Rejecting P2 leads to unphysical resultsand to a conflict with a generalization of P2, a principle P3. It is thus madeplausible that the standard expression of QM completeness must be revised. Anabsolutely explicit form of the axioms is provided, including a precise form ofthe projection postulate. An appropriate expression for QM completeness,reflecting the restrictions of the Gleason and Kochen-Specker theorems isproposed.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "A wireless network in which packets are broadcast to a group of receiversthrough use of a random access protocol is considered in this work. Therelation to previous work on networks of interacting queues is discussed andsubsequently, the stability and throughput regions of the system are analyzedand presented. A simple network of two source nodes and two destination nodesis considered first. The broadcast service process is analyzed assuming achannel that allows for packet capture and multipacket reception. In this smallnetwork, the stability and throughput regions are observed to coincide. Thesame problem for a network with N sources and M destinations is considerednext. The channel model is simplified in that multipacket reception is nolonger permitted. Bounds on the stability region are developed using theconcept of stability rank and the throughput region of the system is comparedto the bounds. Our results show that as the number of destination nodesincreases, the stability and throughput regions diminish. Additionally, aprevious conjecture that the stability and throughput regions coincide for anetwork of arbitrarily many sources is supported for a broadcast scenario bythe results presented in this work.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present general relativistic correction terms appearing in Newton'sgravity to the second-order perturbations of cosmological fluids. In ourprevious work we have shown that to the second-order perturbations, the densityand velocity perturbation equations of general relativistic zero-pressure,irrotational, single-component fluid in a flat background coincide exactly withthe ones known in Newton's theory. Here, we present the general relativisticsecond-order correction terms arising due to (i) pressure, (ii)multi-component, (iii) background curvature, and (iv) rotation. In case ofmulti-component zero-pressure, irrotational fluids under the flat background,we effectively do not have relativistic correction terms, thus the relativisticresult again coincides with the Newtonian ones. In the other three cases wegenerally have pure general relativistic correction terms. In case of pressure,the relativistic corrections appear even in the level of background and linearperturbation equations. In the presence of background curvature, or rotation,pure relativistic correction terms directly appear in the Newtonian equationsof motion of density and velocity perturbations to the second order. In thesmall-scale limit (far inside the horizon), relativistic equations includingthe rotation coincide with the ones in Newton's gravity.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The goal of this paper is to construct invariant dynamical objects for a (notnecessarily invertible) smooth self map of a compact manifold. We prove aresult that takes advantage of differences in rates of expansion in the termsof a sheaf cohomological long exact sequence to create unique lifts of finitedimensional invariant subspaces of one term of the sequence to invariantsubspaces of the preceding term. This allows us to take invariant cohomologicalclasses and under the right circumstances construct unique currents of a giventype, including unique measures of a given type, that represent those classesand are invariant under pullback. A dynamically interesting self map may have aplethora of invariant measures, so the uniquess of the constructed currents isimportant. It means that if local growth is not too big compared to the growthrate of the cohomological class then the expanding cohomological class givessufficient \"marching orders\" to the system to prohibit the formation of anyother such invariant current of the same type (say from some local dynamicalsubsystem). Because we use subsheaves of the sheaf of currents we giveconditions under which a subsheaf will have the same cohomology as the sheafcontaining it. Using a smoothing argument this allows us to show that the sheafcohomology of the currents under consideration can be canonically identifiedwith the deRham cohomology groups. Our main theorem can be applied in both thesmooth and holomorphic setting.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "In several classes of particle physics models -- ranging from the classicalMajoron models, to the more recent scenarios of late neutrino masses orMass-Varying Neutrinos -- one or more of the neutrinos are postulated to coupleto a new light scalar field. As a result of this coupling, neutrinos in theearly universe instead of streaming freely could form a self-coupled fluid,with potentially observable signatures in the Cosmic Microwave Background andthe large scale structure of the universe. We re-examine the constraints onthis scenario from the presently available cosmological data and investigatethe sensitivity expected from the Planck satellite. In the first case, we findthat the sensitivity strongly depends on which piece of data is used. The SDSSMain sample data, combined with WMAP and other data, disfavors the scenario ofthree coupled neutrinos at about the 3.5$\\sigma$ confidence level, but alsofavors a high number of freely streaming neutrinos, with the best fit at 5.2.If the matter power spectrum is instead taken from the SDSS Large Red Galaxysample, best fit point has 2.5 freely streaming neutrinos, but the scenariowith three coupled neutrinos becomes allowed at $2\\sigma$. In contrast, Planckalone will exclude even a single self-coupled neutrino at the $4.2\\sigma$confidence level, and will determine the total radiation at CMB epoch to$\\Delta N_\\nu^{eff} = ^{+0.5}_{-0.3}$ ($1\\sigma$ errors). We investigate therobustness of this result with respect to the details of Planck's detector.This sensitivity to neutrino free-streaming implies that Planck will be capableof probing a large region of the Mass-Varying Neutrino parameter space. Planckmay also be sensitive to a scale of neutrino mass generation as high as 1 TeV.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "A library of C functions yielding exact solutions of potential and fluxinfluences due to uniform surface distribution of singularities on flattriangular and rectangular elements has been developed. This library, ISLES,has been used to develop the neBEM solver that is both precise and fast insolving a wide range of problems of scientific and technological interest. Herewe present the exact expressions proposed for computing the influence ofuniform singularity distributions on triangular elements and illustrate theiraccuracy. We also present a study concerning the time taken to evaluate theselong and complicated expressions \\textit{vis a vis} that spent in carrying outsimple quadratures. Finally, we solve a classic benchmark problem inelectrostatics, namely, estimation of the capacitance of a unit square plateraised to unit volt. For this problem, we present the estimated values ofcapacitance and compare them successfully with some of the most accurateresults available in the literature. In addition, we present the variation ofthe charge density close to the corner of the plate for various degrees ofdiscretization. The variations are found to be smooth and converging. This isin clear contrast to the criticism commonly leveled against usual BEM solvers.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Red supergiant stars represent a key phase in the evolution of massive stars.Recent radiative hydrodynamic simulations suggest that their atmospheres may bethe location of large-scale convective motions. As supergiant convection isexpected to generate supersonic motions and shocks, we seek constraints onthese atmospheric motions and their possible relation with mass-loss rates. Wepresent high-resolution, visible spectroscopy of a sample of red supergiants(spectral type M I) and analyse them with a tomographic technique. We observesteep velocity gradients, characterising both upward and downward supersonicmotions, which are time variable on time scales of a few hundred days. Theseconvective motions will generate turbulent pressure, which will stronglydecrease the effective gravity. We suggest that this decrease, combined withradiative pressure on molecular lines, initiate the mass loss in red supergiantstars.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "A state of an excitonic insulator with the electric current is studied.Initially, in the metallic phase, the electrons and holes are assumed to bemoving in the opposite directions, so as the electric current exists. Thisstate is supported by an external condition (the specimen is in an electriccircuit with the current). When the temperature decreases, the transition tothe ordering state due to formation of the electron--hole pairs is possible(similar to the ordinary state of the excitonic insulator). The properties ofthe state at zero temperature are investigated. The spectrum of elementaryexcitations has a gap, and so the conclusion can be made that obtained state issuperconducting one. Thus, depending on the external conditions, excitonicinsulator behaves itself like the insulator or superconductor. That is correctin the limit of strong overlapping of the electron--hole pairs.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We observed 34 comets using the 24 micron camera on the Spitzer SpaceTelescope. Each image contains the nucleus and covers at least 10^6 km of eachcomet's orbit. Debris trails due to mm-sized or larger particles were foundalong the orbits of 27 comets; 4 comets had small-particle dust tails and aviewing geometry that made debris trails impossible to distinguish; and only 3had no debris trail despite favorable observing conditions. There are now 30Jupiter-family comets with known debris trails, of which 22 are reported inthis paper for the first time. The detection rate is >80%, indicating thatdebris trails are a generic feature of short-period comets. By comparison toorbital calculations for particles of a range of sizes ejected over 2 yr priorto observation, we find that particles comprising 4 debris trails are typicallymm-sized while the remainder of the debris trails require particles larger thanthis. The lower-limit masses of the debris trails are typically 10^11 g, andthe median mass loss rate is 2 kg/s. The mass-loss rate in trail particles iscomparable to that inferred from OH production rates and larger than thatinferred from visible-light scattering in comae.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present the first X-ray detection of the very young pulsar PSR J1357-6429(characteristic age of 7.3 kyr) using data from the XMM-Newton and Chandrasatellites. We find that the spectrum is well described by a power-law plusblackbody model, with photon index Gamma=1.4 and blackbody temperature kT=160eV. For the estimated distance of 2.5 kpc, this corresponds to a 2-10 keVluminosity of about 1.2E+32 erg/s, thus the fraction of the spin-down energychanneled by PSR J1357-6429 into X-ray emission is one of the lowest observed.The Chandra data confirm the positional coincidence with the radio pulsar andallow to set an upper limit of 3E+31 erg/s on the 2-10 keV luminosity of acompact pulsar wind nebula. We do not detect any pulsed emission from thesource and determine an upper limit of 30% for the modulation amplitude of theX-ray emission at the radio frequency of the pulsar.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We investigate one of the consequences of the twisted Poincare symmetry. Wederive the charge conservation law and show that the equivalence principle issatisfied in the canonical noncommutative spacetime. We applied the twistedPoincare symmetry to the Weinberg's analysis. To this end, we generalize ourearlier construction of the twisted S matrix \\cite{Bu}, which apply thenoncommutativity to the fourier modes, to the massless fields of integer spins.The transformation formula for the twisted S matrix for the massless fields ofinteger spin has been obtained. For massless fields of spin 1, we obtain theconservation of charge, and the universality of coupling constant for masslessfields of spin 2, which can be interpreted as the equality of gravitationalmass and inertial mass, i.e., the equivalence principle.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We identify plain evaporation of ions as the fundamental loss mechanism outof a multipole ion trap. Using thermalized negative Cl- ions we find that theevaporative loss rate is proportional to a Boltzmann factor. This thermodynamicdescription sheds new light on the dynamics of particles in time-varyingconfining potentials. It specifically allows us to extract the effective depthof the ion trap as the activation energy for evaporation. As a function of therf amplitude we find two distinct regimes related to the stability of motion ofthe trapped ions. For low amplitudes the entire trap allows for stable motionand the trap depth increases with the rf field. For larger rf amplitudes,however, rapid energy transfer from the field to the ion motion can occur atlarge trap radii, which leads to a reduction of the effective trapping volume.In this regime the trap depth decreases again with increasing rf amplitude. Wegive an analytical parameterization of the trap depth for various multipoletraps that allows predictions of the most favorable trapping conditions.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present the analysis of the source counts in the XMM-COSMOS survey usingdata of the first year of XMM-Newton observations. The survey covers ~2 deg^2within the region of sky bounded by 9^h57.5^m<R.A.<10^h03.5^m;1^d27.5^m<DEC<2^d57.5^m with a total net integration time of 504 ks. Using amaximum likelihood algorithm we detected a total of 1390 sources at least inone band. Using Monte Carlo simulations to estimate the sky coverage weproduced the logN-logS relations. These relations have been then derived in the0.5--2 keV, 2--10 keV and 5--10 keV energy bands, down to flux limits of7.2x10^-16 erg cm^-2 s^-1, 4.0x10^-15 erg cm^-2 s^-1 and 9.7x10^-15 erg cm^-2s^-1, respectively. These relations have been compared to previous X-ray surveyand to the most recent X-ray background model finding an excellent agreement.The slightly different normalizations observed in the source counts of COSMOSand previous surveys can be largely explained as a combination of low countingstatistics and cosmic variance introduced by the large scale structure.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We report on the statistics of strong (W_r > 0.15 A) C IV absorbers atz=1.5-3.5 toward high-redshift gamma-ray bursts (GRBs). In contrast with arecent survey for strong Mg II absorption systems at z < 2, we find that thenumber of C IV absorbers per unit redshift dN/dz does not show a significantdeviation from previous surveys using quasi-stellar objects (QSOs) asbackground sources. We find that the number density of C IV toward GRBs isdN/dz(z~1.5)= 2.2 +2.8/-1.4, dN/dz(z~2.5)= 2.3 +1.8/-1.1 and dN/dz(z~3.5)= 1.1+2.6/-0.9. These numbers are consistent with previous C IV surveys using QSOspectra. Binning the entire dataset, we set a 95% c.l. upper limit to theexcess of C IV absorbers along GRB sightlines at twice the incidence observedalong QSO sightlines. Furthermore, the distribution of equivalent widths of theGRB and QSO samples are consistent with being drawn from the same parentpopulation. Although the results for Mg II and C IV absorbers along GRBsightlines appear to contradict one another, we note that the surveys arenearly disjoint: the C IV survey corresponds to higher redshift and more highlyionized gas than the Mg II survey. Nevertheless, analysis on larger statisticalsamples may constrain properties of the galaxies hosting these metals (e.g.mass, dust content) and/or the coherence-length of the gas giving rise to themetal-line absorption.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Human beings like to believe they are in control of their destiny. Thisubiquitous trait seems to increase motivation and persistence, and is probablyevolutionarily adaptive. But how good really is our ability to control? Howsuccessful is our track record in these areas? There is little understanding ofwhen and under what circumstances we may over-estimate or even lose our abilityto control and optimize outcomes, especially when they are the result ofaggregations of individual optimization processes. Here, we demonstrateanalytically using the theory of Markov Chains and by numerical simulations intwo classes of games, the Minority game and the Parrondo Games, that agents whooptimize their strategy based on past information actually perform worse thannon-optimizing agents. In other words, low-entropy (more informative)strategies under-perform high-entropy (or random) strategies. This provides aprecise definition of the \"illusion of control\" in set-ups a priori defined toemphasize the importance of optimization.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We contrast two sets of conditions that govern the transition in whichclassical dynamics emerges from the evolution of a quantum system. The firstwas derived by considering the trajectories seen by an observer (dubbed the``strong'' transition) [Bhattacharya, et al., Phys. Rev. Lett. 85: 4852(2000)], and the second by considering phase-space densities (the ``weak''transition) [Greenbaum, et al., Chaos 15, 033302 (2005)]. On the face of itthese conditions appear rather different. We show, however, that in thesemiclassical regime, in which the action of the system is large compared to$\\hbar$, and the measurement noise is small, they both offer an essentiallyequivalent local picture. Within this regime, the weak conditions dominatewhile in the opposite regime where the action is not much larger than Planck'sconstant, the strong conditions dominate.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Using the tight-binding model with long-range Coulomb interactions betweenelectrons, we study some of the electronic properties of graphene. The Coulombinteractions are treated with the renormalized-ring-diagram approximation. Byself-consistently solving the integral equations for the Green function, wecalculate the spectral density. The obtained result is in agreement withexperimental observation. In addition, we also compute the density of states,the distribution functions, and the ground-state energy. Within the presentapproximation, we find that the imaginary part of the self-energy fixed at theFermi momentum varies as quadratic in energy close to the chemical potential,regardless the system is doped or not. This result appears to indicate that theelectrons in graphene always behave like a moderately correlated Fermi liquid.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We show that the globular cluster mass function (GCMF) in the Milky Waydepends on cluster half-mass density (rho_h) in the sense that the turnovermass M_TO increases with rho_h while the width of the GCMF decreases. We arguethat this is the expected signature of the slow erosion of a mass function thatinitially rose towards low masses, predominantly through cluster evaporationdriven by internal two-body relaxation. We find excellent agreement between theobserved GCMF -- including its dependence on internal density rho_h, centralconcentration c, and Galactocentric distance r_gc -- and a simple model inwhich the relaxation-driven mass-loss rates of clusters are approximated by-dM/dt = mu_ev ~ rho_h^{1/2}. In particular, we recover the well-knowninsensitivity of M_TO to r_gc. This feature does not derive from a literal``universality'' of the GCMF turnover mass, but rather from a significantvariation of M_TO with rho_h -- the expected outcome of relaxation-drivencluster disruption -- plus significant scatter in rho_h as a function of r_gc.Our conclusions are the same if the evaporation rates are assumed to dependinstead on the mean volume or surface densities of clusters inside their tidalradii, as mu_ev ~ rho_t^{1/2} or mu_ev ~ Sigma_t^{3/4} -- alternativeprescriptions that are physically motivated but involve cluster properties(rho_t and Sigma_t) that are not as well defined or as readily observable asrho_h. In all cases, the normalization of mu_ev required to fit the GCMFimplies cluster lifetimes that are within the range of standard values(although falling towards the low end of this range). Our analysis does notdepend on any assumptions or information about velocity anisotropy in theglobular cluster system.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "In this article we analyze the impact of B-physics and Higgs physics at LEPon standard and non-standard Higgs bosons searches at the Tevatron and the LHC,within the framework of minimal flavor violating supersymmetric models. TheB-physics constraints we consider come from the experimental measurements ofthe rare B-decays b -> s gamma and B_u -> tau nu and the experimental limit onthe B_s -> mu+ mu- branching ratio. We show that these constraints are severefor large values of the trilinear soft breaking parameter A_t, rendering thenon-standard Higgs searches at hadron colliders less promising. On the contrarythese bounds are relaxed for small values of A_t and large values of theHiggsino mass parameter mu, enhancing the prospects for the direct detection ofnon-standard Higgs bosons at both colliders. We also consider the availableATLAS and CMS projected sensitivities in the standard model Higgs searchchannels, and we discuss the LHC's ability in probing the whole MSSM parameterspace. In addition we also consider the expected Tevatron collidersensitivities in the standard model Higgs h -> b bbar channel to show that itmay be able to find 3 sigma evidence in the B-physics allowed regions for smallor moderate values of the stop mixing parameter.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We reanalyse leptogenesis via the out-of-equilibrium decay of the lightestright-handed neutrino in type II seesaw scenarios, taking into accountflavour-dependent effects. In the type II seesaw mechanism, in addition to thetype I seesaw contribution, an additional direct mass term for the lightneutrinos is present. We consider type II seesaw scenarios where thisadditional contribution arises from the vacuum expectation value of a Higgstriplet, and furthermore an effective model-independent approach. Weinvestigate bounds on the flavour-specific decay asymmetries, on the mass ofthe lightest right-handed neutrino and on the reheat temperature of the earlyuniverse, and compare them to the corresponding bounds in the type I seesawframework. We show that while flavour-dependent thermal type II leptogenesisbecomes more efficient for larger mass scale of the light neutrinos, and thebounds become relaxed, the type I seesaw scenario for leptogenesis becomes moreconstrained. We also argue that in general, flavour-dependent effects cannot beignored when dealing with leptogenesis in type II seesaw models.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The search for MSSM Higgs bosons will be an important goal at the LHC. Weanalyze the search reach of the CMS experiment for the heavy neutral MSSM Higgsbosons with an integrated luminosity of 30 or 60 fb^-1. This is done bycombining the latest results for the CMS experimental sensitivities based onfull simulation studies with state-of-the-art theoretical predictions of MSSMHiggs-boson properties. The results are interpreted in MSSM benchmark scenariosin terms of the parameters tan_beta and the Higgs-boson mass scale, M_A. Westudy the dependence of the 5 sigma discovery contours in the M_A-tan_betaplane on variations of the other supersymmetric parameters. The largest effectsarise from a change in the higgsino mass parameter mu, which enters both viahigher-order radiative corrections and via the kinematics of Higgs decays intosupersymmetric particles. While the variation of $\\mu$ can shift theprospective discovery reach (and correspondingly the ``LHC wedge'' region) byabout Delta tan_beta = 10, we find that the discovery reach is rather stablewith respect to the impact of other supersymmetric parameters. Within thediscovery region we analyze the accuracy with which the masses of the heavyneutral Higgs bosons can be determined. We find that an accuracy of 1-4% shouldbe achievable, which could make it possible in favourable regions of the MSSMparameter space to experimentally resolve the signals of the two heavy MSSMHiggs bosons at the LHC.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Using in-medium hadron properties according to the Brown-Rho scaling due tothe chiral symmetry restoration at high densities and considering naturalnessof the coupling constants, we have newly constructed several relativisticmean-field Lagrangians with chiral limits. The model parameters are adjustedsuch that the symmetric part of the resulting equation of state at supra-normaldensities is consistent with that required by the collective flow data fromhigh energy heavy-ion reactions, while the resulting density dependence of thesymmetry energy at sub-saturation densities agrees with that extracted from therecent isospin diffusion data from intermediate energy heavy-ion reactions. Theresulting equations of state have the special feature of being soft atintermediate densities but stiff at high densities naturally. With theseconstrained equations of state, it is found that the radius of a 1.4$M_\\odot$canonical neutron star is in the range of 11.9 km$\\leq$R$\\leq$13.1 km, and themaximum neutron star mass is around 2.0$M_\\odot$ close to the recentobservations.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We analyze the small-scale clustering in \"MegaZ-LRG\", a largephotometric-redshift catalogue of Luminous Red Galaxies extracted from theimaging dataset of the Sloan Digital Sky Survey. MegaZ-LRG, presented in acompanion paper, spans the redshift range 0.4 < z < 0.7 with an r.m.s. redshifterror dz ~ 0.03(1+z), covering 5,914 deg^2 to map out a total cosmic volume 2.5h^-3 Gpc^3. In this study we use 380,000 photometric redshifts to measuresignificant deviations from the canonical power-law fit to the angularcorrelation function in a series of narrow redshift slices, in which weconstruct volume-limited samples. These deviations are direct signatures of themanner in which these galaxies populate the underlying network of dark matterhaloes. We cleanly delineate the separate contributions of the \"1-halo\" and\"2-halo\" clustering terms and fit our measurements by parameterizing the halooccupation distribution N(M) of the galaxies. Our results are successfully fitby a \"central\" galaxy contribution with a \"soft\" transition from zero to onegalaxies, combined with a power-law \"satellite\" galaxy component, the slope ofwhich is a strong function of galaxy luminosity. The large majority of galaxiesare classified as central objects of their host dark matter haloes rather thansatellites in more massive systems. The effective halo mass of MegaZ-LRGgalaxies lies in the range log_10 (M_eff / h^-1 M_sol) = 13.61 - 13.8(increasing with redshift, assuming large-scale normalization sigma_8 = 0.8)for corresponding number densities in the range n_g = 5.03 - 0.56 x 10^-4 h^3Mpc^-3. Our results confirm the usefulness of the halo model for gainingphysical insight into the patterns of galaxy clustering.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "This thesis considers two different aspects of string theory, the tensionlesslimit of the string and supersymmetric sigma models. The tensionless limit isused to find a IIB supergravity background generated by a tensionless string.Quantization of the tensionless string in a pp-wave background is performed andthe tensionless limit is found to commute with quantization. Further, the sigmamodel with N=(2,2) extended world-sheet supersymmetry is considered and therequirement on the target space to have a bi-Hermitean geometry is reviewed. Itis shown that the equivalence between bi-Hermitean geometry and generalizedKahler follows, in this context, from the equivalence between the Lagrangian-and Hamiltonian formulation of the model. Moreover, the explicit T-dualitytransformation in the Hamiltonian formulation of the sigma model is constructedand shown to be a symplectomorphism. Under certain assumptions, the amount ofextended supersymmetry present in the sigma model is shown to be preservedunder T-duality. Further, by requiring N=(2,2) extended supersymmetry in afirst order formulation of the sigma model an intriguing geometrical structurearises and in a special case generalized complex geometry is found to becontained in the new framework.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "A problem which has recently attracted research attention is that ofestimating the distribution of flow sizes in internet traffic. On high trafficlinks it is sometimes impossible to record every packet. Researchers haveapproached the problem of estimating flow lengths from sampled packet data intwo separate ways. Firstly, different sampling methodologies can be tried tomore accurately measure the desired system parameters. One such method is thesample-and-hold method where, if a packet is sampled, all subsequent packets inthat flow are sampled. Secondly, statistical methods can be used to ``invert''the sampled data and produce an estimate of flow lengths from a sample.  In this paper we propose, implement and test two variants on thesample-and-hold method. In addition we show how the sample-and-hold method canbe inverted to get an estimation of the genuine distribution of flow sizes.Experiments are carried out on real network traces to compare standard packetsampling with three variants of sample-and-hold. The methods are compared fortheir ability to reconstruct the genuine distribution of flow sizes in thetraffic.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Hayashi and Carthew (Nature 431 [2004], 647) have shown that the packing ofcone cells in the Drosophila retina resembles soap bubble packing, and thatchanging E- and N-cadherin expression can change this packing, as well as cellshape.  The analogy with bubbles suggests that cell packing is driven by surfaceminimization. We find that this assumption is insufficient to model theexperimentally observed shapes and packing of the cells based on their cadherinexpression. We then consider a model in which adhesion leads to a surfaceincrease, balanced by cell cortex contraction. Using the experimentallyobserved distributions of E- and N-cadherin, we simulate the packing and cellshapes in the wildtype eye. Furthermore, by changing only the correspondingparameters, this model can describe the mutants with different numbers ofcells, or changes in cadherin expression.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present a ground based photometry of the low-temperature contact binary BBPeg. We collected all times of mid-eclipses available in literature andcombined them with those obtained in this study. Analyses of the data indicatea period increase of 3.0(1) x 10^{-8} days/yr. This period increase of BB Pegcan be interpreted in terms of the mass transfer 2.4 x 10^{-8} Ms yr^{-1} fromthe less massive to the more massive component. The physical parameters havebeen determined as Mc = 1.42 Ms, Mh = 0.53 Ms, Rc = 1.29 Rs, Rh = 0.83 Rs, Lc =1.86 Ls, and Lh = 0.94 Ls through simultaneous solution of light and of theradial velocity curves. The orbital parameters of the third body, that orbitsthe contact system in an eccentric orbit, were obtained from the periodvariation analysis. The system is compared to the similar binaries in theHertzsprung-Russell and Mass-Radius diagram.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We define angles from-to and between infinite dimensional subspaces of aHilbert space, inspired by the work of E. J. Hannan, 1961/1962 for generalcanonical correlations of stochastic processes. The spectral theory ofselfadjoint operators is used to investigate the properties of the angles,e.g., to establish connections between the angles corresponding to orthogonalcomplements. The classical gaps and angles of Dixmier and Friedrichs arecharacterized in terms of the angles. We introduce principal invariantsubspaces and prove that they are connected by an isometry that appears in thepolar decomposition of the product of corresponding orthogonal projectors.Point angles are defined by analogy with the point operator spectrum. We boundthe Hausdorff distance between the sets of the squared cosines of the anglescorresponding to the original subspaces and their perturbations. We show thatthe squared cosines of the angles from one subspace to another can beinterpreted as Ritz values in the Rayleigh-Ritz method, where the formersubspace serves as a trial subspace and the orthogonal projector of the lattersubspace serves as an operator in the Rayleigh-Ritz method. The Hausdorffdistance between the Ritz values, corresponding to different trial subspaces,is shown to be bounded by a constant times the gap between the trial subspaces.We prove a similar eigenvalue perturbation bound that involves the gap squared.Finally, we consider the classical alternating projectors method and proposeits ultimate acceleration, using the conjugate gradient approach. Thecorresponding convergence rate estimate is obtained in terms of the angles. Weillustrate a possible acceleration for the domain decomposition method with asmall overlap for the 1D diffusion equation.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We apply the technique of parameter-splitting to existing cosmological datasets, to check for a generic failure of dark energy models. Given a dark energyparameter, such as the energy density Omega_Lambda or equation of state w, wesplit it into two meta-parameters with one controlling geometrical distances,and the other controlling the growth of structure. Observational data spanningType Ia Supernovae, the cosmic microwave background (CMB), galaxy clustering,and weak gravitational lensing statistics are fit without requiring the twometa-parameters to be equal. This technique checks for inconsistency betweendifferent data sets, as well as for internal inconsistency within any one dataset (e.g., CMB or lensing statistics) that is sensitive to both geometry andgrowth. We find that the cosmological constant model is consistent with currentdata. Theories of modified gravity generally predict a relation between growthand geometry that is different from that of general relativity.Parameter-splitting can be viewed as a crude way to parametrize the space ofsuch theories. Our analysis of current data already appears to put sharp limitson these theories: assuming a flat universe, current data constrain thedifference Omega_Lambda(geom) - Omega_Lambda(grow) to be -0.0044 +/- 0.0058(68% C.L.); allowing the equation of state w to vary, the difference w(geom) -w(grow) is constrained to be 0.37 +/- 0.37 (68% C.L.). Interestingly, theregion w(grow) > w(geom), which should be generically favored by theories thatslow structure formation relative to general relativity, is quite restricted bydata already. We find w(grow) < -0.80 at 2 sigma. As an example, the best-fitflat Dvali-Gabadadze-Porrati (DGP) model approximated by our parametrizationlies beyond the 3 sigma contour for constraints from all the data sets.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Let $X$ be a compact K\\\"ahler manifold and $\\om$ a smooth closed form ofbidegree $(1,1)$ which is nonnegative and big. We study the classes ${\\mathcalE}_{\\chi}(X,\\om)$ of $\\om$-plurisubharmonic functions of finite weightedMonge-Amp\\`ere energy. When the weight $\\chi$ has fast growth at infinity, thecorresponding functions are close to be bounded.  We show that if a positive Radon measure is suitably dominated by theMonge-Amp\\`ere capacity, then it belongs to the range of the Monge-Amp\\`ereoperator on some class ${\\mathcal E}_{\\chi}(X,\\om)$. This is done byestablishing a priori estimates on the capacity of sublevel sets of thesolutions.  Our result extends U.Cegrell's and S.Kolodziej's results and puts them into aunifying frame. It also gives a simple proof of S.T.Yau's celebrated a priori${\\mathcal C}^0$-estimate.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "After the work of Gladman et al. (1998), it is now assessed that manyirregular satellites are orbiting around Uranus. Despite many studies have beenperformed in past years, very few is know for the light-curves of these objectsand inconsistencies are present between colours derived by different authors.This situation motivated our effort to improve both the knowledge of coloursand light curves. We present and discuss time series observations of Sycorax,Prospero, Stephano, Setebos and Trinculo, five faint irregular satellites ofUranus, carried out at VLT, ESO Paranal (Chile) in the nights between 29 and 30July, 2005 and 25 and 30 November, 2005. We derive light curves for Sycorax andProspero and colours for all of these these bodies. For Sycorax we obtaincolours B-V =0.839 +/- 0.014, V-R = 0.531 +/- 0.005 and a light curve which issuggestive of a periodical variation with period about 3.6 hours and amplitudeabout 0.067 +/- 0.004 mag. The periods and colours we derive for Sycorax are inagreement with our previous determination in 1999 using NTT. We derive also alight-curve for Prospero which suggests an amplitude of about 0.2 mag and aperiodicity of about 4 hours. However, the sparseness of our data, prevents amore precise characterization of the light-curves, and we can not determinewether they are one-peaked or two-peaked. Hence, these periods and amplitudeshave to be considered preliminary estimates. As for Setebos, Stephano andTrinculo the present data do not allow to derive any unambiguous periodicity,despite Setebos displays a significant variability with amplitude about aslarge as that of Prospero. Colours for Prospero, Setebos, Stephano and Trinculoare in marginal agreement with the literature.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Low energy supersymmetric models provide a solution to the hierarchy problemand also have the necessary ingredients to solve two of the most outstandingissues in cosmology: the origin of dark matter and baryonic matter. One of themost attractive features of this framework is that the relevant physicalprocesses are related to interactions at the weak scale and therefore may betested in collider experiments in the near future. This is true for the MinimalSupersymmetric Standard Model (MSSM) as well as for its extension with theaddition of one singlet chiral superfield, the so-called nMSSM. It has beenrecently shown that within the nMSSM an elegant solution to both the problem ofbaryogenesis and dark matter may be found, that relies mostly on the mixing ofthe singlet sector with the Higgs sector of the theory. In this work we reviewthe nMSSM model constraints from cosmology and present the associated colliderphenomenology at the LHC and the ILC. We show that the ILC will efficientlyprobe the neutralino, chargino and Higgs sectors, allowing to confrontcosmological observations with computations based on collider measurements. Wealso investigate the prospects for a direct detection of dark matter and theconstraints imposed by the current bounds of the electron electric dipolemoment in this model.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We investigate the effect of planetary rotation on the transit spectrum of anextrasolar giant planet. During ingress and egress, absorption features arisingfrom the planet's atmosphere are Doppler shifted by of order the planet'srotational velocity (~1-2 km/s) relative to where they would be if the planetwere not rotating. We focus in particular on the case of HD209458b, which oughtto be at least as good a target as any other known transiting planet. ForHD209458b, this shift should give rise to a small net centroid shift of ~60cm/s on the stellar absorption lines. Using a detailed model of thetransmission spectrum due to a rotating star transited by a rotating planetwith an isothermal atmosphere, we simulate the effect of the planet's rotationon the shape of the spectral lines, and in particular on the magnitude of theirwidth and centroid shift. We then use this simulation to determine the expectedsignal-to-noise ratio for distinguishing a rotating from a non-rotating planet,and assess how this S/N scales with various parameters of HD209458b. We findthat with a 6 m telescope, an equatorial rotational velocity of ~2 km/s couldbe detected with a S/N~5 by accumulating the signal over many transits over thecourse of several years. With a 30 m telescope, the time required to make sucha detection reduces to less than 2 months.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We carry out the non-perturbative renormalization of the chromo-magneticoperator in Heavy Quark Effective Theory. At order 1/m of the expansion, theoperator is responsible for the mass splitting between the pseudoscalar andvector B mesons. We obtain its two-loop anomalous dimension in a Schr\"odingerfunctional scheme by successive one-loop conversions to the lattice MS schemeand the MS-bar scheme. We then compute the scale evolution of the operatornon-perturbatively in the N_f=0 theory between $\\mu \\approx 0.3$ GeV and $\\mu\\approx 100$ GeV, where contact is made with perturbation theory. The overallrenormalization factor that converts the bare lattice operator to itsrenormalization group invariant form is given for the Wilson gauge action andtwo standard discretizations of the heavy-quark action. As an application, wefind that this factor brings the previous quenched predictions of the B* - Bmass splitting closer to the experimental value than found with a perturbativerenormalization. The same renormalization factor is applicable to thespin-dependent potentials of Eichten and Feinberg.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present predictions for the evolution of the galaxy luminosity function,number counts and redshift distributions in the IR based on the Lambda-CDMcosmological model. We use the combined GALFORM semi-analytical galaxyformation model and GRASIL spectrophotometric code to compute galaxy SEDsincluding the reprocessing of radiation by dust. The model, which is the sameas that in Baugh et al (2005), assumes two different IMFs: a normal solarneighbourhood IMF for quiescent star formation in disks, and a very top-heavyIMF in starbursts triggered by galaxy mergers. We have shown previously thatthe top-heavy IMF seems to be necessary to explain the number counts of faintsub-mm galaxies. We compare the model with observational data from the SPITZERSpace Telescope, with the model parameters fixed at values chosen beforeSPITZER data became available. We find that the model matches the observedevolution in the IR remarkably well over the whole range of wavelengths probedby SPITZER. In particular, the SPITZER data show that there is strong evolutionin the mid-IR galaxy luminosity function over the redshift range z ~ 0-2, andthis is reproduced by our model without requiring any adjustment of parameters.On the other hand, a model with a normal IMF in starbursts predicts far toolittle evolution in the mid-IR luminosity function, and is therefore excluded.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present results of the analysis of cometary X-ray spectra with an extendedversion of our charge exchange emission model (Bodewits et al. 2006). We haveapplied this model to the sample of 8 comets thus far observed with the ChandraX-ray observatory and ACIS spectrometer in the 300-1000 eV range. The surveyedcomets are C/1999 S4 (LINEAR), C/1999 T1 (McNaught-Hartley), C/2000 WM1(LINEAR), 153P/2002 (Ikeya-Zhang), 2P/2003 (Encke), C/2001 Q4 (NEAT), 9P/2005(Tempel 1) and 73P/2006-B (Schwassmann-Wachmann 3) and the observations includea broad variety of comets, solar wind environments and observationalconditions. The interaction model is based on state selective, velocitydependent charge exchange cross sections and is used to explore how cometaryX-ray emission depend on cometary, observational and solar windcharacteristics. It is further demonstrated that cometary X-ray spectra mainlyreflect the state of the local solar wind. The current sample of Chandraobservations was fit using the constrains of the charge exchange model, andrelative solar wind abundances were derived from the X-ray spectra. Ouranalysis showed that spectral differences can be ascribed to different solarwind states, as such identifying comets interacting with (I) fast, cold wind,(II), slow, warm wind and (III) disturbed, fast, hot winds associated withinterplanetary coronal mass ejections. We furthermore predict the existence ofa fourth spectral class, associated with the cool, fast high latitude wind.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Surviving in a diverse environment requires corresponding organism responses.At the cellular level, such adjustment relies on the transcription factors(TFs) which must rapidly find their target sequences amidst a vast amount ofnon-relevant sequences on DNA molecules. Whether these transcription factorslocate their target sites through a 1D or 3D pathway is still a matter ofspeculation. It has been suggested that the optimum search time is when theprotein equally shares its search time between 1D and 3D diffusions. In thispaper, we study the above problem using a Monte Carlo simulation by consideringa very simple physical model. A 1D strip, representing a DNA, with a number oflow affinity sites, corresponding to non-target sites, and high affinity sites,corresponding to target sites, is considered and later extended to a 2D strip.We study the 1D and 3D exploration pathways, and combinations of the two modesby considering three different types of molecules: a walker that randomly walksalong the strip with no dissociation; a jumper that represents dissociation andthen re-association of a TF with the strip at later time at a distant site; anda hopper that is similar to the jumper but it dissociates and thenre-associates at a faster rate than the jumper. We analyze the finalprobability distribution of molecules for each case and find that TFs canlocate their targets fast enough even if they spend 15% of their search timediffusing freely in the solution. This indeed agrees with recent experimentalresults obtained by Elf et al. 2007 and is in contrast with theoreticalexpectation.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We examine the structure of the post-shock region in supernova remnants(SNRs). The ``shock transition zone'' is set up by charge transfer andionization events between atoms and ions, and has a width $\\sim 10^{15}$cm$^{-2}$ $n^{-1}_0$, where $n_0$ is the total pre-shock density (includingboth atoms and ions). For Balmer-dominated SNRs with shock velocity $v_s\\gtrsim 1000$ km s$^{-1}$, the Rankine-Hugoniot conditions for ion velocity andtemperature are obeyed instantly, leaving the full width at half-maximum (FWHM)of the broad H$\\alpha$ line versus $v_s$ relation intact. However, the spatialvariation in the post-shock densities is relevant to the problem of Ly$\\alpha$resonant scattering in young, core-collapse SNRs. Both two- (pre-shock atomsand ions) and three-component (pre-shock atoms, broad neutrals and ions) modelsare considered. We compute the spatial emissivities of the broad ($\\xi_b$) andnarrow ($\\xi_n$) H$\\alpha$ lines; a calculation of these emissivities in SN1006 is in general agreement with the computed ones of Raymond et al. (2007).The (dimensionless) spatial shift, $\\Theta_{\\rm{shift}}$, between the centroidsof $\\xi_b$ and $\\xi_n$ is unique for a given shock velocity and $f_{\\rm{ion}}$,the pre-shock ion fraction. Measurements of $\\Theta_{\\rm{shift}}$ can be usedto constrain $n_0$.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Clear evidence for symplectic symmetry in low-lying states of $^{12}$C and$^{16}$O is reported. Eigenstates of $^{12}$C and $^{16}$O, determined withinthe framework of the no-core shell model using the JISP16 $NN$ realisticinteraction, typically project at the 85-90% level onto a few of the mostdeformed symplectic basis states that span only a small fraction of the fullmodel space. The results are nearly independent of whether the bare orrenormalized effective interactions are used in the analysis. The outcomeconfirms Elliott's \\SU{3} model which underpins the symplectic scheme, andabove all, points to the relevance of a symplectic no-core shell model that canreproduce experimental B(E2) values without effective charges as well asdeformed spatial modes associated with clustering phenomena in nuclei.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We use strongly coupled lattice QED with two flavors of massless staggeredfermions to model the physics of pions in two-flavor massless QCD. Our modelhas the right chiral symmetries and can be studied efficiently with clusteralgorithms. In particular we can tune the strength of the QCD anomaly and thusstudy its effects on the chiral phase transition. Our study confirms the widelyaccepted view point that the chiral phase transition is first order in theabsence of the anomaly. Turning on the anomaly weakens the transition and turnsit second order at a critical anomaly strength. The anomaly strength at thetricritical point is characterized using $r = (M_{\\eta'}-M_{\\pi})/\\rho_{\\eta'}$where $M_{\\eta'}, M_{\\pi}$ are the screening masses of the anomalous andregular pions and $\\rho_{\\eta'}$ is the mass-scale that governs the low energyfluctuations of the anomalous symmetry. We estimate that $r \\sim 7 $ in ourmodel. This suggests that a strong anomaly at the two-flavor QCD chiral phasetransition is necessary to wash out the first order transition.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "By making use of the finite-temperature real-time static potential that wasintroduced and computed to leading non-trivial order in Hard Thermal Loopresummed perturbation theory in recent work, and solving numerically aSchr\\\"odinger-type equation, we estimate the quarkonium (in practice,bottomonium) contribution to the spectral function of the electromagneticcurrent in hot QCD. The spectral function shows a single resonance peak whichbecomes wider and then disappears as the temperature is increased beyond 450MeV or so. This behaviour can be compared with recently attempted latticereconstructions of the same quantity, based on the ``maximum entropy method'',which generically show several peaks. We also specify the dependence of ourresults on the spatial momentum of the electromagnetic current, as well as onthe baryon chemical potential characterising the hot QCD plasma.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We study the infrared (IR) properties of galaxies in the cluster MS 1054-03at z=0.83 by combining MIPS 24 micron data with spectra of more than 400galaxies and a very deep K-band selected catalog. 19 IR cluster members areselected spectroscopically, and an additional 15 are selected by theirphotometric redshifts. We derive the IR luminosity function of the cluster andfind strong evolution compared to the similar-mass Coma cluster. The bestfitting Schechter function gives L*_{IR}=11.49 +0.30/-0.29 L_sun with a fixedfaint end slope, about one order of magnitude larger than that in Coma. Therate of evolution of the IR luminosity from Coma to MS 1054-03 is consistentwith that found in field galaxies, and it suggests that some internalmechanism, e.g., the consumption of the gas fuel, is responsible for thegeneral decline of the cosmic star formation rate (SFR) in differentenvironments. The mass-normalized integrated SFR within 0.5R_200 in MS 1054-03also shows evolution compared with other rich clusters at lower redshifts, butthe trend is less conclusive if the mass selection effect is considered. Anonnegligible fraction (13%) of cluster members, are forming stars actively andthe overdensity of IR galaxies is about 20 compared to the field. It isunlikely that clusters only passively accrete star forming galaxies from thesurrounding fields and have their star formation quenched quickly afterward;instead, many cluster galaxies still have large amounts of gas, and their starformation may be enhanced by the interaction with the cluster.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The X-ray transient XMMU J174716.1-281048 was serendipitously discovered withXMM-Newton in 2003. It lies about 0.9 degrees off the Galactic Centre and itsspectrum shows a high absorption (~8 x 10E22 cm^(-2)). Previous X-rayobservations of the source field performed in 2000 and 2001 did not detect thesource, indicative of a quiescent emission at least two orders of magnitudefainter. The low luminosity during the outburst (~5 x 10E34 erg/s at 8 kpc)indicates that the source is a member of the ``very faint X-ray transients''class. On 2005 March 22nd the INTEGRAL satellite caught a possible type-I X-rayburst from the new INTEGRAL source IGR J17464-2811, classified as fast X-raytransient. This source was soon found to be positionally coincident, within theuncertainties, with XMMU J174716.1-281048. Here we report data analysis of theX-ray burst observed with the IBIS and JEM-X telescopes and confirm the type-Iburst nature. We also re-analysed XMM-Newton and Chandra archival observationsof the source field. We discuss the implications of these new findings,particularly related to the source distance as well as the sourceclassification.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The phase of Super-Soft-Source (SSS) emission of the sixth recorded outburstof the recurrent nova RS Oph was observed twice with Chandra and once withXMM-Newton. The observations were taken on days 39.7, 54.0, and 66.9 afteroutburst. We confirm a 35-sec period on day 54.0 and found that it originatesfrom the SSS emission and not from the shock. We discus the bound-freeabsorption by neutral elements in the line of sight, resonance absorption linesplus self-absorbed emission line components, collisionally excited emissionlines from the shock, He-like intersystem lines, and spectral changes during anepisode of high-amplitude variability. We find a decrease of the oxygen K-shellabsorption edge that can be explained by photoionization of oxygen. Theabsorption component has average velocities of -1286+-267 km/s on day 39.7 andof -771+-65 km/s on day 66.9. The wavelengths of the emission line componentsare consistent with their rest wavelengths as confirmed by measurements ofnon-self absorbed He-like intersystem lines. We have evidence that these linesoriginate from the shock rather than the outer layers of the outflow and may bephotoexcited in addition to collisional excitations. We found collisionallyexcited emission lines that are fading at wavelengths shorter than 15A thatoriginate from the radiatively cooling shock. On day 39.5 we find a systematicblue shift of -526+-114 km/s from these lines. We found anomalous He-like f/iratios which indicates either high densities or significant UV radiation nearthe plasma where the emission lines are formed. During the phase of strongvariability the spectral hardness light curve overlies the total light curvewhen shifted by 1000sec. This can be explained by photoionization of neutraloxygen in the line of sight if the densities of order 10^{10}-10^{11} cm^{-3}.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "A coarse-grained computational procedure based on the Finite Element Methodis proposed to calculate the normal modes and mechanical response of proteinsand their supramolecular assemblies. Motivated by the elastic network model,proteins are modeled as homogeneous isotropic elastic solids with volumedefined by their solvent-excluded surface. The discretized Finite Elementrepresentation is obtained using a surface simplification algorithm thatfacilitates the generation of models of arbitrary prescribed spatialresolution. The procedure is applied to compute the normal modes of a mutant ofT4 phage lysozyme and of filamentous actin, as well as the critical Eulerbuckling load of the latter when subject to axial compression. Results comparefavorably with all-atom normal mode analysis, the Rotation Translation Blocksprocedure, and experiment. The proposed methodology establishes a computationalframework for the calculation of protein mechanical response that facilitatesthe incorporation of specific atomic-level interactions into the model,including aqueous-electrolyte-mediated electrostatic effects. The procedure isequally applicable to proteins with known atomic coordinates as it is toelectron density maps of proteins, protein complexes, and supramolecularassemblies of unknown atomic structure.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The conventional magnetic induction equation that governs hydromagneticdynamo action is transformed into an equivalent integral equation system. Anadvantage of this approach is that the computational domain is restricted tothe region occupied by the electrically conducting fluid and to its boundary.This integral equation approach is first employed to simulate kinematic dynamosexcited by Beltrami-like flows in a finite cylinder. The impact of externallyadded layers around the cylinder on the onset of dynamo actions isinvestigated. Then it is applied to simulate dynamo experiments withincylindrical geometry including the von Karman sodium (VKS) experiment and theRiga dynamo experiment. A modified version of this approach is utilized toinvestigate magnetic induction effects under the influence of externallyapplied magnetic fields which is also important to measure the proximity of agiven dynamo facility to the self-excitation threshold.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We discuss in detail the problem of counting BPS gauge invariant operators inthe chiral ring of quiver gauge theories living on D-branes probing generictoric CY singularities. The computation of generating functions that includecounting of baryonic operators is based on a relation between the baryoniccharges in field theory and the Kaehler moduli of the CY singularities. A studyof the interplay between gauge theory and geometry shows that given geometricalsectors appear more than once in the field theory, leading to a notion of\"multiplicities\". We explain in detail how to decompose the generating functionfor one D-brane into different sectors and how to compute their relevantmultiplicities by introducing geometric and anomalous baryonic charges. ThePlethystic Exponential remains a major tool for passing from one D-brane toarbitrary number of D-branes. Explicit formulae are given for few examples,including C^3/Z_3, F_0, and dP_1.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Onsager conjectured that weak solutions of the Euler equations forincompressible fluids in 3D conserve energy only if they have a certain minimalsmoothness, (of order of 1/3 fractional derivatives) and that they dissipateenergy if they are rougher. In this paper we prove that energy is conserved forvelocities in the function space $B^{1/3}_{3,c(\\NN)}$. We show that this spaceis sharp in a natural sense. We phrase the energy spectrum in terms of theLittlewood-Paley decomposition and show that the energy flux is controlled bylocal interactions. This locality is shown to hold also for the helicity flux;moreover, every weak solution of the Euler equations that belongs to$B^{2/3}_{3,c(\\NN)}$ conserves helicity. In contrast, in two dimensions, thestrong locality of the enstrophy holds only in the ultraviolet range.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The plethora of recent cosmologically relevant data has indicated that ouruniverse is very well fit by a standard Friedmann-Lema\\^{i}tre-Robertson-Walker(FLRW) model, with $\\Omega_{M} \\approx 0.27$ and $\\Omega_{\\Lambda} \\approx0.73$ -- or, more generally, by nearly flat FLRW models with parameters closeto these values. Additional independent cosmological information, particularlythe maximum of the angular-diameter (observer-area) distance and the redshiftat which it occurs, would improve and confirm these results, once sufficientprecise Supernovae Ia data in the range $1.5 < z < 1.8$ become available. Weobtain characteristic FLRW closed functional forms for $C = C(z)$ and$\\hat{M}_0 = \\hat{M}_0(z)$, the angular-diameter distance and the density persource counted, respectively, when $\\Lambda \\neq 0$, analogous to those we havefor $\\Lambda = 0$. More importantly, we verify that for flat FLRW models$z_{max}$ -- as is already known but rarely recognized -- the redshift of$C_{max}$, the maximum of the angular-diameter-distance, uniquely gives$\\Omega_{\\Lambda}$, the amount of vacuum energy in the universe, independentlyof $H_0$, the Hubble parameter. For non-flat models determination of both$z_{max}$ and $C_{max}$ gives both $\\Omega_{\\Lambda}$ and $\\Omega_M$, theamount of matter in the universe, as long as we know $H_0$ independently.Finally, determination of $C_{max}$ automatically gives a very simpleobservational criterion for whether or not the universe is flat -- presumingthat it is FLRW.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We introduce a simple nearest-neighbor spin model with multiple metastablephases, the number and decay pathways of which are explicitly controlled by theparameters of the system. With this model we can construct, for example, asystem which evolves through an arbitrarily long succession of metastablephases. We also construct systems in which different phases may nucleatecompetitively from a single initial phase. For such a system, we present ageneral method to extract from numerical simulations the individual nucleationrates of the nucleating phases. The results show that the Ostwald rule, whichpredicts which phase will nucleate, must be modified probabilistically when thenew phases are almost equally stable. Finally, we show that the nucleation rateof a phase depends, among other things, on the number of other phasesaccessible from it.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We investigate the relation between thermodynamic and dynamic properties ofan associating lattice gas (ALG) model. The ALG combines a three dimensionallattice gas with particles interacting through a soft core potential andorientational degrees of freedom. From the competition between the directionalattractive forces and the soft core potential results two liquid phases, doublecriticality and density anomaly. We study the mobility of the molecules in thismodel by calculating the diffusion constant at a constant temperature, $D$. Weshow that $D$ has a maximum at a density $\\rho_{max}$ and a minimum at adensity $\\rho_{min}<\\rho_{max}$. Between these densities the diffusivitydiffers from the one expected for normal liquids. We also show that in thepressure-temperature phase-diagram the line of extrema in diffusivity is closeto the liquid-liquid critical point and it is partially inside the temperatureof maximum density (TMD) line.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "In the present paper we study two qubit entanglement in the most general$XYZ$ Heisenberg magnetic chain with (non)homogeneous magnetic fields and theDM anisotropic antisymmetric exchange interaction, arising from the spin-orbitcoupling . The model includes all known results as particular cases, for bothantiferromagnetic and ferromagnetic $XX, XY, XXX, XXZ, XYZ$ chains. Theconcurrence of two qubit thermal entanglement and its dependence on anisotropicparameters, external magnetic field and temperature are studied in details. Wefound that in all cases, inclusion of the DM interaction, which is responsiblefor weak ferromagnetism in mainly antiferromagnetic crystals and spinarrangement in low symmetry magnets, creates (when it does not exist) orstrengthens (when it exists) entanglement in $XYZ$ spin chain. This impliesexistence of a relation between arrangement of spins and entanglement, in whichthe DM coupling plays an essential role. It suggests also that anisotropicantisymmetric exchange interaction could be an efficient control parameter ofentanglement in the general $XYZ$ case.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We propose a new field-theoretic framework for formulating thenon-relativistic quantum mechanics of D particles in a Fock space of U(N)Yang-Mills theories with all different N in a unified way. D-particle fieldoperators, creating and annihilating a D particle and hence changing N one byone, are defined. The base space of these D-particle fields is a (complex)vector space of infinite dimensions. The gauge invariance of Yang-Mills quantummechanics is reinterpreted as a quantum-statistical symmetry, which is takeninto account by setting up a novel algebraic and projective structure in theformalism. Ordinary physical observables of Yang-Mills theory, obeying thestandard algebra, are expressed as bilinear forms of the D-particle fields.Together with the open-closed string duality, our new formulation suggests atrinity of three different but mutually dual viewpoints in string theory.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Author offers and researches a new, cheap method for the extraction offreshwater from the Earth atmosphere. The suggected method is fundamentallydictinct from all existing methods that extract freshwater from air. All otherindustrial methods extract water from a saline water source (in most cases fromseawater). This new method may be used at any point in the Earth except PolarZones. It does not require long-distance freshwater transportation. If seawateris not utilized for increasing its productivity, this inexpensive new method isvery environment-friendly. The author method has two working versions: (1) thefirst variant the warm (hot) atmospheric air is lifted by the inflatable tubein a high altitude and atmospheric steam is condenced into freswater: (2) inthe second version, the warm air is pumped 20-30 meters under the sea-surface.In the first version, wind and solar heating of air are used for causing airflow. In version (2) wind and propeller are used for causing air movment.  The first method does not need energy, the second needs a small amount.Moreover, in variant (1) the freshwater has a high pressure (>30 or more atm.)and can be used for production of energy such as electricity and in that waythe freshwater cost is lower. For increasing the productivity the seawater isinjected into air and solar air heater may be used. The solar air heaterproduces a huge amount of electricity as a very powerful electricity generationplant. The offered electricity installation in 100 - 200 times cheaper than anycommon electric plant of equivalent output.  Key words: Extraction freshwater, method of getting freshwater, receivingenergy from atmosphere, powerful renewal electric plant.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present a simple implementation of the dynamical mean-field theoryapproach to the electronic structure of strongly correlated materials. Thisimplementation achieves full self-consistency over the charge density, takinginto account correlation-induced changes to the total charge density andeffective Kohn-Sham Hamiltonian. A linear muffin-tin orbital basis-set is used,and the charge density is computed from moments of the many bodymomentum-distribution matrix. The calculation of the total energy is alsoconsidered, with a proper treatment of high-frequency tails of the Green'sfunction and self-energy. The method is illustrated on two materials withwell-localized 4f electrons, insulating cerium sesquioxide Ce2O3 and thegamma-phase of metallic cerium, using the Hubbard-I approximation to thedynamical mean-field self-energy. The momentum-integrated spectral function andmomentum-resolved dispersion of the Hubbard bands are calculated, as well asthe volume-dependence of the total energy. We show that full self-consistencyover the charge density, taking into account its modification by strongcorrelations, can be important for the computation of both thermodynamical andspectral properties, particularly in the case of the oxide material.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We consider the extent to which future imaging surveys of galaxies candistinguish between dark energy and modified gravity models for the origin ofthe cosmic acceleration. Dynamical dark energy models may have similarexpansion rates as models of modified gravity, yet predict different growth ofstructure histories. We parameterize the cosmic expansion by the twoparameters, $w_0$ and $w_a$, and the linear growth rate of density fluctuationsby Linder's $\\gamma$, independently. Dark energy models generically predict$\\gamma \\approx 0.55$, while the DGP model $\\gamma \\approx 0.68$. To determineif future imaging surveys can constrain $\\gamma$ within 20 percent (or$\\Delta\\gamma<0.1$), we perform the Fisher matrix analysis for a weak lensingsurvey such as the on-going Hyper Suprime-Cam (HSC) project. Under thecondition that the total observation time is fixed, we compute the Figure ofMerit (FoM) as a function of the exposure time $\\texp$. We find that thetomography technique effectively improves the FoM, which has a broad peakaround $\\texp\\simeq {\\rm several}\\sim 10$ minutes; a shallow and wide survey ispreferred to constrain the $\\gamma$ parameter. While $\\Delta\\gamma < 0.1$cannot be achieved by the HSC weak-lensing survey alone, one can improve theconstraints by combining with a follow-up spectroscopic survey like WFMOSand/or future CMB observations.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The frequency distribution of DNA bases A, C, G, T exhibit fractalfluctuations ubiquitous to dynamical systems in nature. The power spectra offractal fluctuations exhibit inverse power law form signifying long-rangecorrelations between local (small-scale) and global (large-scale)perturbations. The author has developed a general systems theory based onclassical statistical physics for fractal fluctuations which predicts that theprobability distribution of eddy amplitudes and the variance (square of eddyamplitude)spectrum of fractal fluctuations follow the universal Boltzmanninverse power law expressed as a function of the golden mean. The modelpredicted distribution is very close to statistical normal distribution forfluctuations within two standard deviations from the mean and exhibits a fatlong tail. In this paper it is shown that DNA base CG frequency distribution inTakifugu rubripes (Puffer fish) Genome Release 4 exhibit universal inversepower law form consistent with model prediction. The observed long-rangecorrelations in the DNA bases implies that the non-coding 'junk' or 'selfish'DNA which appear to be redundant, may also contribute to the efficientfunctioning of the protein coding DNA, a result supported by recent studies.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We consider power allocation algorithms for fixed-rate transmission overNakagami-m non-ergodic block-fading channels with perfect transmitter andreceiver channel state information and discrete input signal constellationsunder both short- and long-term power constraints. Optimal power allocationschemes are shown to be direct applications of previous results in theliterature. We show that the SNR exponent of the optimal short-term scheme isgiven by the Singleton bound. We also illustrate the significant gainsavailable by employing long-term power constraints. Due to the nature of theexpressions involved, the complexity of optimal schemes may be prohibitive forsystem implementation. We propose simple sub-optimal power allocation schemeswhose outage probability performance is very close to the minimum outageprobability obtained by optimal schemes.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "I show that several observable properties of bursting neutron stars in metrictheories of gravity can be calculated using only conservation laws, Killingsymmetries, and the Einstein equivalence principle, without requiring thevalidity of the general relativistic field equations. I calculate, inparticular, the gravitational redshift of a surface atomic line, the touchdownluminosity of a radius-expansion burst, which is believed to be equal to theEddington critical luminosity, and the apparent surface area of a neutron staras measured during the cooling tails of bursts. I show that, for a generalmetric theory of gravity, the apparent surface area of a neutron star dependson the coordinate radius of the stellar surface and on its gravitationalredshift in the exact same way as in general relativity. On the other hand, theEddington critical luminosity depends also on an additional parameter thatmeasures the degree to which the general relativistic field equations aresatisfied. These results can be used in conjunction with current and futurehigh-energy observations of bursting neutron stars to test general relativityin the strong-field regime.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The MuCap experiment is a high-precision measurement of the rate for thebasic electroweak process of muon capture, mu- + p -> n + nu . The experimentalapproach is based on an active target consisting of a time projection chamber(TPC) operating with pure hydrogen gas. The hydrogen has to be kept extremelypure and at a stable pressure. A Circulating Hydrogen Ultrahigh PurificationSystem was designed at the Petersburg Nuclear Physics Institute (PNPI) tocontinuously clean the hydrogen from impurities. The system is based on anadsorption cryopump to stimulate the hydrogen flow and on a cold adsorbent forthe hydrogen cleaning. It was installed at the Paul Scherrer Institute (PSI) in2004 and performed reliably during three experiment runs. During several monthslong operating periods the system maintained the hydrogen purity in thedetector on the level of 20 ppb for moisture, which is the main contaminant,and of better than 7 ppb and 5 ppb for nitrogen and oxygen, respectively. Thepressure inside the TPC was stabilized to within 0.024% of 10 bar at a hydrogenflow rate of 3 standard liters per minute.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The classical Euler's problem on stationary configurations of elastic rodwith fixed endpoints and tangents at the endpoints is considered as aleft-invariant optimal control problem on the group of motions of atwo-dimensional plane $\\E(2)$.  The attainable set is described, existence and boundedness of optimalcontrols are proved. Extremals are parametrized by Jacobi's elliptic functionsof natural coordinates induced by the flow of the mathematical pendulum onfibers of the cotangent bundle of $\\E(2)$.  The group of discrete symmetries of Euler's problem generated by reflectionsin the phase space of the pendulum is studied. The corresponding Maxwell pointsare completely described via the study of fixed points of this group. As aconsequence, an upper bound on cut points in Euler's problem is obtained.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present here a detailed study of the behaviour of a three dimensionalBrownian motor based on cold atoms in a double optical lattice [P. Sjolund etal., Phys. Rev. Lett. 96, 190602 (2006)]. This includes both experiments andnumerical simulations of a Brownian particle. The potentials used are spatiallyand temporally symmetric, but combined spatiotemporal symmetry is broken byphase shifts and asymmetric transfer rates between potentials. The diffusion ofatoms in the optical lattices is rectified and controlled both in direction andspeed along three dimensions. We explore a large range of experimentalparameters, where irradiances and detunings of the optical lattice lights arevaried within the dissipative regime. Induced drift velocities in the order ofone atomic recoil velocity have been achieved.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "An automated magnetometer suitable for long lasting measurement under stableand controllable experimental conditions has been implemented. The device isbased on Coherent Population Trapping (CPT) produced by a multi-frequencyexcitation. CPT resonance is observed when a frequency comb, generated by diodelaser current modulation, excites Cs atoms confined in a$\\pi/4\\times(2.5)^2\\times1 \\textrm{cm}^3$, 2 Torr $N_2$ buffered cell. A fullyoptical sensor is connected through an optical fiber to the laser head allowingfor truly remote sensing and minimization of the field perturbation. A detailedanalysis of the CPT resonance parameters as a function of the optical detuninghas been made in order to get high sensitivity measurements. The magnetic fieldmonitoring performances and the best sensitivity obtained in a balanceddifferential configuration of the sensor are presented.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Plasmas in an accretion flow are heated by MHD turbulence generated throughthe magneto-rotational instability. The viscous stress driving the accretion isintimately connected to the microscopic processes of turbulence dissipation. Weshow that, in a few well-observed black hole accretion systems, there iscompelling observational evidence of efficient electron heating by turbulenceor collective plasma effects in low accretion states, when Coulomb collisionsare not efficient enough to establish a thermal equilibrium between electronsand ions at small radii. However, charged particles reach a thermal equilibriumwith their kind much faster than with others through Coulomb collisions, atwo-temperature accretion flow is expected. We consider a Keplerian accretionflow with a constant mass accretion rate in the pseudo-Newtonian gravitationalpotential and take into account the bremsstrahlung, synchrotron, and inverseComptonization cooling processes. The critical mass accretion rate, below whichthe two-temperature solution may exist, is determined by the cooling processesand the collisional energy exchanges between electrons and ions and has veryweak dependence on the collision-less heating of electrons by turbulence, whichbecomes more important at lower accretion rates. Collision-less heating ofelectrons by MHD turbulence can no longer be ignored in quantitativeinvestigations of these systems.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We consider a three dimensional system consisting of a large number of smallspherical particles, distributed in a range of sizes and heights (with uniformdistribution in the horizontal direction). Particles move vertically at asize-dependent terminal velocity. They are either allowed to merge wheneverthey cross or there is a size ratio criterion enforced to account for collisionefficiency. Such a system may be described, in mean field approximation, by theSmoluchowski kinetic equation with a differential sedimentation kernel, used tostudy e.g. rain initiation and particle distributions in the atmosphere. Wesolve the kinetic equation analytically to obtain steady state and self-similarsolutions in time and in height, using methods borrowed from weak turbulencetheory. Analytical results are compared with direct numerical simulations (DNS)of moving and merging particles, and a good agreement is found.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We consider anisotropic magnetized cosmologies filled with conductive plasmafluid and study the implications of metric perturbations that propagateparallel to the ambient magnetic field. It is known that in the first order(linear) approximation with respect to the amplitude of the perturbations noelectric field and density perturbations arise. However, when we consider thenon-linear coupling of the metric perturbations with their temporalderivatives, certain classes of solutions can induce steeply increasing in timeelectric field perturbations. This is verified both numerically andanalytically. The source of these perturbations can be either high-frequencyquantum vacuum fluctuations, driven by the cosmological pump field, in theearly stages of the evolution of the Universe or astrophysical processes or anon-linear isotropization process of an initially anisotropic cosmologicalspacetime.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "An extensive literature exists describing various techniques for theevaluation of Hankel determinants. The prevailing methods such as Dodgsoncondensation, continued fraction expansion, LU decomposition, all produceproduct formulas when they are applicable. We mention the classic case of theHankel determinants with binomial entries ${3k+2 \\choose k}$ and those withentries ${3k \\choose k}$; both of these classes of Hankel determinants haveproduct form evaluations. The intermediate case, ${3k+1 \\choose k}$ has notbeen evaluated. There is a good reason for this: these latter determinants donot have product form evaluations.  In this paper we evaluate the Hankel determinant of ${3k+1 \\choose k}$. Theevaluation is a sum of a small number of products, an almost product.  The method actually provides more, and as applications, we present thesalient points for the evaluation of a number of other Hankel determinants withpolynomial entries, along with product and almost product form evaluations atspecial points.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "A new catalogue of extended radio sources has been prepared based onarcminute-resolution 1420 MHz images from the Canadian Galactic Plane Survey(CGPS). The new catalogue provides both 1420 MHz and 408 MHz flux densitymeasurements on sources found near the Galactic plane in the second quadrant ofour Galaxy. In addition cross-identifications are made with other major radiocatalogues and information is provided to facilitate the recovery of CGPS imagedata associated with each catalogued source. Numerous new radio sources areidentified and the catalogue provides a comprehensive summary of both newlydiscovered and previously known HII regions and supernova remnants in the outerGalaxy. The catalogue should be of use both for synoptic studies of Galacticstructure and for placing higher resolution observations, at radio and otherwavelengths, in context.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We have investigated the possibility of direct tests of little Higgs modelsincorporating triplet Higgs neutrino mass mechanism at LHC experiments. We haveperformed Monte Carlo studies of Drell-Yan pair production of doubly chargedHiggs boson \\Phi^{++} followed by its leptonic decays which branching ratiosare fixed from the neutrino oscillation data. We propose appropriate selectionrules for the four-lepton signal, including reconstructed taus, which areoptimized for the discovery of \\Phi^{++} with the lowest LHC luminosity. As theStandard Model background can be effectively eliminated, an important aspect ofour study is the correct statistical treatment of the LHC discovery potential.Adding detection efficiencies and measurement errors to the Monte Carloanalyses, \\Phi^{++} can be discovered up to the mass 250 GeV in the first yearof LHC, and 700 GeV mass is reachable for the integrated luminosity L=30fb^{-1}.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "A new class of Erbium doped glasses with compositions xNa2O - (60-x)PbCl2 -40P2O5 (x=0, 10, 20 and 30) were fabricated and characterized for opticalproperties. Absorption spectra were analyzed for important Judd-Ofeltparameters from the integrated intensities of various Er3+ glass absorptionbands. Photoluminescence (PL) and its decay behavior studies were carried outfor the transition 4I13/2 -> 4I15/2. A systematic correlation between theJudd-Ofelt parameter {omega}2 and the covalent nature of the glass matrix wasobserved, due to increased role of bridging oxygens in the glass network. ThePL broadness and life times of 4I13/2_> 4I15/2 transition were typically in therange of 40-60nm and 2.13-2.5ms respectively. These glasses broadly showed hightransparency, high refractive index, shorter life times and, most importantly,these glasses were found to be capable of being doped with largerconcentrations of Er3+ (up to 4 wt%). Increase of Er3+ concentration resultedin the increase in PL line-widths with no significant effect of concentrationquenching, indicating that these glasses are suitable for opticalfibre/waveguide amplifiers.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We consider the interpretation of tetrad fields as reference frames inspacetime. Reference frames may be characterized by an antisymmetricacceleration tensor, whose components are identified as the inertialaccelerations of the frame (the translational acceleration and the frequency ofrotation of the frame). This tensor is closely related togravitoelectromagnetic field quantities. We construct the set of tetrad fieldsadapted to observers that are in free fall in the Schwarzschild spacetime, andshow that the gravitational energy-momentum constructed out of this set oftetrad fields, in the framework of the teleparallel equivalent of generalrelatrivity, vanishes. This result is in agreement with the principle ofequivalence, and may be taken as a condition for a viable definition ofgravitational energy.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The following question is addressed: under what conditions can a strangediffusive process, defined by a semi-dynamical V-Langevin equation or itsassociated Hybrid kinetic equation (HKE), be described by an equivalent purelystochastic process, defined by a Continuous Time Random Walk (CTRW) or by aFractional Differential Equation (FDE)? More specifically, does there exist aclass of V-Langevin equations with long-range (algebraic) velocity temporalcorrelation, that leads to a time-fractional superdiffusive process? The answeris always affirmative in one dimension. It is always negative in twodimensions: any algebraically decaying temporal velocity correlation (with aGaussian spatial correlation) produces a normal diffusive process. Generalconditions relating the diffusive nature of the process to the temporalexponent of the Lagrangian velocity correlation (in Corrsin approximation) arederived.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "This is a sequel to [Ca01]=math.AG/0110051. We define the bimeromorphic {\\itcategory} of geometric orbifolds. These interpolate between (compact K\\\" ahler)manifolds and such manifolds with logarithmic structure. These geometricorbifolds are considered from the point of view of their geometry, and thusequipped with the usual invariants of varieties: morphisms and bimeromorphicmaps, differential forms, fundamental groups and universal covers, fields ofdefinition and rational points. The most elementary properties, directlyadapted from the case of varieties without orbifold structure, are establishedhere. The arguments of [Ca01] can then be directly adapted to extend the mainstructure results to this orbifold category. We hope to come back to deeperaspects later. The motivation is that the natural frame for the theory ofclassification of compact K\\\" ahler (and complex projective) manifolds includesat least the category of orbifolds, as shown in [Ca01] by the fonctorialdecomposition of {\\it special} manifolds as tower of orbifolds with either$\\kappa_+=-\\infty$ or $\\kappa=0$, and also, seemingly, by the minimal modelprogram, in which most proofs work only after the adjunction of a \"boundary\".  Also, fibrations enjoy in the bimeromorphic category of geometric orbifoldsextension properties not satisfied in the category of varieties withoutorbifold structure, permitting to express invariants of the total space fromthose of the generic fibre and of the base. For example, the natural sequenceof fundamental groups is exact there; also the total space is special if so arethe generic fibre and the base. This makes this category suitable to liftproperties from orbifolds having either $\\kappa_+=-\\infty$ or $\\kappa=0$ tothose which are special.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Current methods for producing single-walled carbon nanotubes (SWNTs) lead toheterogeneous samples containing mixtures of metallic and semiconductingspecies with a variety of lengths and defects. Optical detection at the singlenanotube level should thus offer the possibility to examine theseheterogeneities provided that both SWNT species are equally well detected.Here, we used photothermal heterodyne detection to record absorption images andspectra of individual SWNTs. Because this photothermal method relies only onlight absorption, it readily detects metallic nanotubes as well as the emissivesemiconducting species. The first and second optical transitions in individualsemicontucting nanotubes have been probed. Comparison between the emission andabsorption spectra of the lowest-lying optical transition reveal mainly smallStokes shifts. Side bands in the near-infrared absorption spectra are observedand assigned to exciton-phonon bound states. No such sidebands are detectedaround the lowest transition of metallic nanotubes.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Max-product belief propagation is a local, iterative algorithm to find themode/MAP estimate of a probability distribution. While it has been successfullyemployed in a wide variety of applications, there are relatively fewtheoretical guarantees of convergence and correctness for general loopy graphsthat may have many short cycles. Of these, even fewer provide exact ``necessaryand sufficient'' characterizations.  In this paper we investigate the problem of using max-product to find themaximum weight matching in an arbitrary graph with edge weights. This is doneby first constructing a probability distribution whose mode corresponds to theoptimal matching, and then running max-product. Weighted matching can also beposed as an integer program, for which there is an LP relaxation. Thisrelaxation is not always tight. In this paper we show that \\begin{enumerate}\\item If the LP relaxation is tight, then max-product always converges, andthat too to the correct answer. \\item If the LP relaxation is loose, thenmax-product does not converge. \\end{enumerate} This provides an exact,data-dependent characterization of max-product performance, and a preciseconnection to LP relaxation, which is a well-studied optimization technique.Also, since LP relaxation is known to be tight for bipartite graphs, ourresults generalize other recent results on using max-product to find weightedmatchings in bipartite graphs.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We consider the discretization  y(t+\\epsilon)=y(t-\\epsilon)+2\\epsilon\\big(1-y(t)^{2}\\big),  $\\epsilon>0$ a small parameter, of the logistic differential equation$y'=2\\big(1-y^{2}\\big)$, which can also be seen as a discretization of thesystem  {y'=2\\big(1-v^{2}\\big),  v'= 2\\big(1-y^{2}\\big).  This system has two saddle points at $A=(1,1)$, $B=(-1, -1)$ and there existstable and unstable manifolds. We will show that the stable manifold$W_{s}^{+}$ of the point $A=(1,1)$ and the unstable manifold $W_{i}^{-}$ of thepoint $B=(-1, -1)$ for the discretization do not coincide. The verticaldistance between these two manifolds is exponentially small but not zero, inparticular we give an asymptotic estimate of this distance. For this purpose wewill use a method adapted from the paper of Sch\\\"afke-Volkmer \\cite{SV} usingformal series and accurate estimates of the coefficients.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "This paper follows in the tradition of direct-action versions ofelectromagnetism having the aim of avoiding a balance of infinities wherein amechanical mass offsets an infinite electromagnetic mass so as to arrive at afinite observed value. Given that, in this respect the direct-action approachedultimately failed because its initial exclusion of self-action was found to beuntenable in the relativistic domain, this paper continues the traditionconsidering instead a version of electromagnetism wherein mechanical action isexcluded and self-action is retained. It is shown that the resulting theory iseffectively interacting due to the presence of infinite forces. A vehicle forthe investigation is a pair of classical point charges in a positronium-likearrangement for which the orbits are found to be self-sustaining and naturallyquantized.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Annealed importance sampling is a means to assign equilibrium weights to anonequilibrium sample that was generated by a simulated annealing protocol. Theweights may then be used to calculate equilibrium averages, and also serve asan ``adiabatic signature'' of the chosen cooling schedule. In this paper wedemonstrate the method on the 50-atom dileucine peptide, showing thatequilibrium distributions are attained for manageable cooling schedules. Forthis system, as naively implemented here, the method is modestly more efficientthan constant temperature simulation. However, the method is worth consideringwhenever any simulated heating or cooling is performed (as is often done at thebeginning of a simulation project, or during an NMR structure calculation), asit is simple to implement and requires minimal additional CPU expense.Furthermore, the naive implementation presented here can be improved.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Random walks on expander graphs were thoroughly studied, with the importantmotivation that, under some natural conditions, these walks mix quickly andprovide an efficient method of sampling the vertices of a graph. Alon,Benjamini, Lubetzky and Sodin studied non-backtracking random walks on regulargraphs, and showed that their mixing rate may be up to twice as fast as that ofthe simple random walk. As an application, they showed that the maximal numberof visits to a vertex, made by a non-backtracking random walk of length $n$ ona high-girth $n$-vertex regular expander, is typically $(1+o(1))\\frac{\\logn}{\\log\\log n}$, as in the case of the balls and bins experiment. They furtherasked whether one can establish the precise distribution of the visits such awalk makes.  In this work, we answer the above question by combining a generalized form ofBrun's sieve with some extensions of the ideas in Alon et al. Let $N_t$ denotethe number of vertices visited precisely $t$ times by a non-backtracking randomwalk of length $n$ on a regular $n$-vertex expander of fixed degree and girth$g$. We prove that if $g=\\omega(1)$, then for any fixed $t$, $N_t/n$ istypically $\\frac{1}{\\mathrm{e}t!}+o(1)$. Furthermore, if $g=\\Omega(\\log\\logn)$, then $N_t/n$ is typically $\\frac{1+o(1)}{\\mathrm{e}t!}$ uniformly on all$t \\leq (1-o(1))\\frac{\\log n}{\\log\\log n}$ and 0 for all $t \\geq(1+o(1))\\frac{\\log n}{\\log\\log n}$. In particular, we obtain the above resulton the typical maximal number of visits to a single vertex, with an improvedthreshold window. The essence of the proof lies in showing that variablescounting the number of visits to a set of sufficiently distant vertices areasymptotically independent Poisson variables.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The photon box thought experiment can be considered a forerunner of theEPR-experiment: by performing suitable measurements on the box it is possibleto ``prepare'' the photon, long after it has escaped, in either of twocomplementary states. Consistency requires that the corresponding boxmeasurements be complementary as well. At first sight it seems, however, thatthese measurements can be jointly performed with arbitrary precision: theypertain to different systems (the center of mass of the box and an internalclock, respectively). But this is deceptive. As we show by explicitcalculation, although the relevant quantities are simultaneously measurable,they develop non-vanishing commutators when calculated back to the time ofescape of the photon. This justifies Bohr's qualitative arguments in a preciseway; and it illustrates how the details of the dynamics conspire to guaranteethe requirements of complementarity. In addition, our calculations exhibit a``fine structure'' in the distribution of the uncertainties over thecomplementary quantities: depending on when the box measurement is performed,the resulting quantum description of the photon differs. This brings us closeto the argumentation of the later EPR thought experiment.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "Density-functional theory requires ever better exchange-correlation (xc)functionals for the ever more precise description of many-body effects onelectronic structure. Universal constraints on the xc energy are importantingredients in the construction of improved functionals. Here we investigateone such universal property of xc functionals: the Lieb-Oxford lower bound onthe exchange-correlation energy, $E_{xc}[n] \\ge -C \\int d^3r n^{4/3}$, where$C\\leq C_{LO}=1.68$. To this end, we perform a survey of available exact ornear-exact data on xc energies of atoms, ions, molecules, solids, and somemodel Hamiltonians (the electron liquid, Hooke's atom and the Hubbard model).All physically realistic density distributions investigated are consistent withthe tighter limit $C \\leq 1$. For large classes of systems one can obtainclass-specific (but not fully universal) similar bounds. The Lieb-Oxford boundwith $C_{LO}=1.68$ is a key ingredient in the construction of modern xcfunctionals, and a substantial change in the prefactor $C$ will haveconsequences for the performance of these functionals.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The aim of the present paper is to provide a global presentation of thetheory of special Finsler manifolds. We introduce and investigate globally (orintrinsically, free from local coordinates) many of the most important and mostcommonly used special Finsler manifolds: locally Minkowskian, Berwald,Landesberg, general Landesberg, $P$-reducible, $C$-reducible,semi-$C$-reducible, quasi-$C$-reducible, $P^{*}$-Finsler, $C^{h}$-recurrent,$C^{v}$-recurrent, $C^{0}$-recurrent, $S^{v}$-recurrent, $S^{v}$-recurrent ofthe second order, $C_{2}$-like, $S_{3}$-like, $S_{4}$-like, $P_{2}$-like,$R_{3}$-like, $P$-symmetric, $h$-isotropic, of scalar curvature, of constantcurvature, of $p$-scalar curvature, of $s$-$ps$-curvature. The globaldefinitions of these special Finsler manifolds are introduced. Variousrelationships between the different types of the considered special Finslermanifolds are found. Many local results, known in the literature, are provedglobally and several new results are obtained. As a by-product, interestingidentities and properties concerning the torsion tensor fields and thecurvature tensor fields are deduced. Although our investigation is entirelyglobal, we provide; for comparison reasons, an appendix presenting a localcounterpart of our global approach and the local definitions of the specialFinsler spaces considered.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "By combining the local density approximation (LDA) with dynamical mean fieldtheory (DMFT), we report a systematic analysis of the spectral properties of$\\delta$-plutonium with varying $5f$ occupancy. The LDA Hamiltonian isextracted from a tight-binding (TB) fit to full-potential linearized augmentedplane-wave (FP-LAPW) calculations. The DMFT equations are solved by the exactquantum Monte Carlo (QMC) method and the Hubbard-I approximation. We have shownfor the first time the strong sensitivity of the spectral properties to the$5f$ occupancy, which suggests using this occupancy as a fitting parameter inaddition to the Hubbard $U$. By comparing with PES data, we conclude that the``open shell'' $5f^{5}$ configuration gives the best agreement, resolving thecontroversy over $5f$ ``open shell'' versus ``close shell'' atomicconfigurations in $\\delta$-Pu.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "The extraction of the weak phase $\\alpha$ from $B\\to\\pi\\pi$ decays has beencontroversial from a statistical point of view, as the frequentist vs. bayesianconfrontation shows. We analyse several relevant questions which have notdeserved full attention and pervade the extraction of $\\alpha$.Reparametrization Invariance proves appropriate to understand those issues. Weshow that some Standard Model inspired parametrizations can be senseless orinadequate if they go beyond the minimal Gronau and London assumptions: thesingle weak phase $\\alpha$ just in the $\\Delta I=3/2$ amplitudes, the isospinrelations and experimental data. Beside those analyses, we extract $\\alpha$through the use of several adequate parametrizations, showing that there is norelevant discrepancy between frequentist and bayesian results. The mostrelevant information, in terms of $\\alpha$, is the exclusion of values around$\\alpha\\sim \\pi/4$; this result is valid in the presence of arbitrary NewPhysics contributions to the $\\Delta I=1/2$ piece.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "We present observations of the (1,1), (2,2), (4,4) and (5,5) inversiontransitions of para-ammonia (NH3) and 24 GHz continuum, taken with theAustralia Telescope Compact Array toward 21 southern Galactic hot molecularcores traced by 6.7 GHz methanol maser emission. We detect NH3(1,1) emissiontoward all 21 regions and 24 GHz continuum emission toward 12 of the regions,including 6 with no reported 8 GHz continuum counterparts. In total, we findthe 21 regions contain 41 NH3(1,1) cores. We extract characteristic spectra forevery core at each of the NH3 transitions and present both integrated intensitymaps and channel maps for each region. The NH3(4,4)+(5,5) emission is alwaysunresolved and found at the maser position indicating that the methanol masersare found at the warmest part of the core. We observe large asymmetries in theNH3(1,1) hyperfine line profiles and conclude this is due to a number of dense,small clumps within the beam. We derive properties of the ionised gas and findthe 24 GHz continuum sources not detected at 8 GHz are always coincident withboth NH3 and methanol masers in contrast to those detected at 8 + 24 GHz whichare generally offset from the methanol masers. We investigate the possibilitythat the former may be hyper-compact HII regions. Finally, we separate thecores into five groups, based on their association with NH3, methanol maser andcontinuum emission. From the different physical properties of the cores in thegroups, we discuss the possibility that these groups may represent cores atdifferent evolutionary stages of the massive star formation process.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "A discrete tensegrity framework can be thought of as a graph in Euclideann-space where each edge is of one of three types: an edge with a fixed length(bar) or an edge with an upper (cable) or lower (strut) bound on its length.Roth and Whiteley, in their 1981 paper \"Tensegrity Frameworks\", showed that incertain cases, the struts and cables can be replaced with bars when analyzingthe framework for infinitesimal rigidity. In that case we call the tensegrity\"bar equivalent\". In specific, they showed that if there exists a set ofpositive weights, called a positive \"stress\", on the edges such that theweighted sum of the edge vectors is zero at every vertex, then the tensegrityis bar equivalent.  In this paper we consider an extended version of the tensegrity framework inwhich the vertex set is a (possibly infinite) set of points in Euclideann-space and the edgeset is a compact set of unordered pairs of vertices. Theseare called \"continuous tensegrities\". We show that if a continuous tensegrityhas a strictly positive stress, it is bar equivalent and that it has asemipositive stress if and only if it is partially bar equivalent. We also showthat if a tensegrity is minimally bar equivalent (it is bar equivalent butremoving any open set of edges makes it no longer so), then it has a strictlypositive stress.  In particular, we examine the case where the vertices form a rectifiablecurve and the possible motions of the curve are limited to local isometries ofit. Our methods provide an attractive proof of the following result: There isno locally arclength preserving motion of a circle that increases any antipodaldistance without decreasing some other one.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "In this paper, we investigate a new waveform for UWB systems obtained by thecombination of Orthogonal Frequency Division Multiplex (OFDM) and Code DivisionMultiple Access (CDMA). The proposed system, called Spread Spectrum -Multi-Carrier - Multiple Access (SS-MC-MA) turns out to be a judicious solutionto combat frequency selectivity and narrowband interferers, and to manage thecoexistence of several users and piconets. It is shown that the addition of adegree of freedom brought by the spreading component of SS-MC-MA allows tooptimize jointly the assignment of the number of used codes and coding rates inorder to make the system more robust. Through simulations, it is demonstratedthat the new system can outperform Multi-Band OFDM Alliance (MBOA) for low datarates and is able to provide wider range of rates.", "output": ""}
{"instruction": "what is the prompt that generates the input?", "input": "For many years various asymmetrical profiles of different spectral linesemitted from solar flares have been frequently observed. These asymmetries orline shifts are caused predominantly by vertical mass motions in flaring layersand they provide a good diagnostics for plasma flows during solar flares. Thereare many controversial results of observations and theoretical analysis ofplasma flows in solar chromospheric flares. The main difficulty is theinterpretation of line shifts or asymmetries. For many years, methods based onbisector techniques were used but they give a reliable results only for somespecific conditions and in most cases cannot be applied. The most promisingapproach is to use the non-LTE techniques applied for flaring atmosphere. Thecalculation of synthetic line profiles is performed with the radiative transfertechniques and the assumed physical conditions correspond to flaringatmosphere. I will present an overview of different observations andinterpretations of line asymmetries in chromospheric flares. I will explainwhat we have learnt about the chromospheric evaporation in the frame ofhydrodynamical models as well as reconnection models. A critical review will bedone on the classical methods used to derive Doppler-shifts for optically thickchomospheric lines. In particular, details on the new approach for interpretingchromospheric line asymmetries based on the non-LTE techniques will bepresented.", "output": ""}