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.


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.


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.


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.


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.


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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.


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.


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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.


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.


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.


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.


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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.


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.


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.


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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.


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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.


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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.


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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.


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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.


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.


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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.


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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.


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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.


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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.


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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.


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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.


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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.


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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.


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$_2$.


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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.


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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.


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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.


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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.


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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.


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.


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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.


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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.


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.


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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.


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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.


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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.


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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.


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.


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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...


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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.


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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.


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.


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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.


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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.


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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.


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.


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.


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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.


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.


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.


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.


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.


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.


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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.


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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.


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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.


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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.


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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.


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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.


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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.


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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.


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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.


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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.


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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.


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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 $q=3$.


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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.


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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.


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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.


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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]


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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.


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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.


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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.


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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.


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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.