Instruction: what is the prompt that generates the input?

Input: Using a semi-analytical model for galaxy formation, combined with a largeN-body simulation, we investigate the origin of the dichotomy among early-typegalaxies. We find that boxy galaxies originate from mergers with a progenitormass ratio $n < 2$ and with a combined cold gas mass fraction $F_{\rm cold} <0.1$. Our model accurately reproduces the observed fraction of boxy systems asa function of luminosity and halo mass, for both central galaxies andsatellites. After correcting for the stellar mass dependence, the properties ofthe last major merger of early-type galaxies are independent of their halomass. This provides theoretical support for the conjecture of Pasquali et al(2007) that the stellar mass of an early-type galaxy is the main parameter thatgoverns its isophotal shape. We argue that the observed dichotomy of early-typegalaxies has a natural explanation within hierarchical structure formation, anddoes not require AGN feedback. Rather, we argue that it owes to the fact thatmore massive systems (i) have more massive progenitors, (ii) assemble later,and (iii) have a larger fraction of early-type progenitors. Each of these threetrends causes the cold gas mass fraction of the progenitors of more massiveearly-types to be lower, so that their last major merger was dryer. Finally,our model predicts that (i) less than 10 percent of all early-type galaxiesform in major mergers that involve two early-type progenitors, (ii) more than95 percent of all boxy early-type galaxies with $M_* < 2 \times 10^{10} h^{-1}\Msun$ are satellite galaxies, and (iii) about 70 percent of all low massearly-types do not form a supermassive black hole binary at their last majormerger. The latter may help to explain why low mass early-types have centralcusps, while their massive counterparts have cores.


Instruction: what is the prompt that generates the input?

Input: Color confinement and chiral symmetry specify some important territory forthe study of hadronic physics. Any hadron can be defined as a color-singletcomposite system of qurks and gluons, the fundamental fields of qcd, while thelandscape of the hadronic spectrum is dominated by the fact that two quarkflavors, u and d, are characterized by masses small compared to the fundamentalscale of this theory. Measurements sensitive to the orbital angular momenta ofthe color constituents of the nucleon display the interplay of chiral dynamicsand confinement in a unique manner. This pageant can be explored by anevaluation, within the context of the Georgi-Manohar chiral quark model, of thenormalization of the orbital structure functions and the normalization of theBoer-Mulders functions for different quark flavors. The resolution structuresin the chiral quark model represent an evaluation of Collins functions for aconfined system defined by the quantum numbers of the nucleon in theconstituent quark model. The orbital structure functions for antiquarks canalso be specified within the basic framework of this approach while thenormalization of the gluon orbital structure function requires some additionalassumptions.


Instruction: what is the prompt that generates the input?

Input: We present observations and modeling of a lunar occultation of thedust-enshrouded carbon star AFGL 5440. The observations were made over acontinuous range of wavelengths from 1 - 4um with a high-speedspectrophotometer designed expressly for this purpose. We find that theoccultation fringes cannot be fit by any single-size model. We use the DUSTYradiative transfer code to model a circumstellar shell and fit both theobserved occultation light curves and the spectral energy distributiondescribed in the literature. We find a strong constraint on the inner radius ofthe dust shell, Tmax = 950 K +/- 50K, and optical depth at 5um of 0.5 +/- 0.1.The observations are best fit by models with a density gradient of r^-2 or thegradient derived by Ivezic & Elitzur for a radiatively driven hydrodynamicoutflow. Our models cannot fit the observed IRAS 60um flux without assuming asubstantial abundance of graphite or by assuming a substantially highermass-loss rate in the past.


Instruction: what is the prompt that generates the input?

Input: The blasting of brittle materials with sharp particles is an importantfabrication technology in many industrial processes. In particular, formicro-systems, it allows the production of devices with feature sizes down tofew tens of microns. An important parameter of this process is the surfaceroughness of post-blasted surfaces. In this work the scaling properties ofPyrex glass and silicon surfaces after bombardment with alumina particles isinvestigated. The targets were bombarded at normal incidence using aluminaparticles with two different average sizes, $29\mu m$ and $9\mu m$,respectively. This investigation indicates that the resulting surfaces havemultifractal properties. Applying multifractal detrended fluctuation analysis(MFDFA) allowed us to determine the singularity spectrum of the surfaces. Thisspectrum did not depend on the target material or on the size of the particles.Several parameters quantifying relevant quantities were determined. We arguethat for scales below $5 \mu m$, fracture processes are dominant while at largescales long range correlations are responsible for the multifractal behaviour.


Instruction: what is the prompt that generates the input?

Input: Context: The mass-loss rate is a key parameter of massive stars. Adequatestellar atmosphere models are required for spectral analyses and mass-lossdeterminations. Present models can only account for the inhomogeneity ofstellar winds in the approximation of small-scale structures that are opticallythin. This treatment of ``microclumping'' has led to reducing empiricalmass-loss rates by factors of two and more. Aims: Stellar wind clumps can beoptically thick in spectral lines. We investigate how this ``macroclumping''impacts on empirical mass-loss rates. Methods: The Potsdam Wolf-Rayet (PoWR)model atmosphere code is generalized in the ``formal integral'' to account forclumps that are not necessarily optically thin. Results: Optically thick clumpsreduce the effective opacity. This has a pronounced effect on the emergentspectrum. Our modeling for the O-type supergiant zeta Puppis reveals that theoptically thin H-alpha line is not affected by wind porosity, but that the PVresonance doublet becomes significantly weaker when macroclumping is taken intoaccount. The reported discrepancies between resonance-line andrecombination-line diagnostics can be resolved entirely with the macroclumpingmodeling without downward revision of the mass-loss rate. Conclusions:Mass-loss rates inferred from optically thin emission, such as the H-alpha linein O stars, are not influenced by macroclumping. The strength of opticallythick lines, however, is reduced because of the porosity effects. Therefore,neglecting the porosity in stellar wind modeling can lead to underestimatingempirical mass-loss rates.


Instruction: what is the prompt that generates the input?

Input: Let $C_a$ be the central Cantor set obtained by removing a central intervalof length $1-2a$ from the unit interval, and continuing this processinductively on each of the remaining two intervals. We prove that if $\logb/\log a$ is irrational, then \[ \dim(C_a+C_b) = \min(\dim(C_a) + \dim(C_b),1),\] where $\dim$ is Hausdorff dimension. More generally, given two self-similarsets $K,K'$ in $\RR$ and a scaling parameter $s>0$, if the dimension of thearithmetic sum $K+sK'$ is strictly smaller than $\dim(K)+\dim(K') \le 1$(``geometric resonance''), then there exists $r<1$ such that all contractionratios of the similitudes defining $K$ and $K'$ are powers of $r$ (``algebraicresonance''). Our method also yields a new result on the projections of planarself-similar sets generated by an iterated function system that includes ascaled irrational rotation.


Instruction: what is the prompt that generates the input?

Input: We explore the cosmological content of Salam-Sezgin six dimensionalsupergravity, and find a solution to the field equations in qualitativeagreement with observation of distant supernovae, primordial nucleosynthesisabundances, and recent measurements of the cosmic microwave background. Thecarrier of the acceleration in the present de Sitter epoch is a quintessencefield slowly rolling down its exponential potential. Intrinsic to this model isa second modulus which is automatically stabilized and acts as a source of colddark matter with a mass proportional to an exponential function of thequintessence field (hence realizing VAMP models within a String context).However, any attempt to saturate the present cold dark matter component in thismanner leads to unacceptable deviations from cosmological data -- a numericalstudy reveals that this source can account for up to about 7% of the total colddark matter budget. We also show that (1) the model will support a de Sitterenergy in agreement with observation at the expense of a miniscule breaking ofsupersymmetry in the compact space; (2) variations in the fine structureconstant are controlled by the stabilized modulus and are negligible; (3)``fifth''forces are carried by the stabilized modulus and are short range; (4)the long time behavior of the model in four dimensions is that of aRobertson-Walker universe with a constant expansion rate (w = -1/3). Finally,we present a String theory background by lifting our six dimensionalcosmological solution to ten dimensions.


Instruction: what is the prompt that generates the input?

Input: All maximal supergravities in four space-time dimensions are presented. Theungauged Lagrangians can be encoded in an E_7(7)\Sp(56,R)/GL(28) matrixassociated with the freedom of performing electric/magnetic dualitytransformations. The gauging is defined in terms of an embedding tensor whichencodes the subgroup of E_7(7) that is realized as a local invariance. Thisembedding tensor may imply the presence of magnetic charges which requirecorresponding dual gauge fields. The latter can be incorporated by using arecently proposed formulation that involves tensor gauge fields in the adjointrepresentation of E_7(7). In this formulation the results take a universal formirrespective of the electric/magnetic duality basis. We present the generalclass of supersymmetric and gauge invariant Lagrangians and discuss a number ofapplications.


Instruction: what is the prompt that generates the input?

Input: By their star content, the galaxies split out into a red and a bluepopulation; their color index peaked around u-r=2.5 or u-r=1, respectively,quantifies the ratio of the blue stars newly formed from cold galactic gas, tothe redder ones left over by past generations. On the other hand, uponaccreting substantial gas amounts the central massive black holes energizeactive galactic nuclei (AGNs); here we investigate whether these show asimilar, and possibly related, bimodal partition as for current accretionactivity relative to the past. To this aim we use an updated semianalyticmodel; based on Monte Carlo simulations, this follows with a large statisticsthe galaxy assemblage, the star generations and the black hole accretions inthe cosmological framework over the redshift span from z=10 to z=0. We test oursimulations for yielding in close detail the observed split of galaxies into ared, early and a blue, late population. We find that the black hole accretionactivities likewise give rise to two source populations: early, bright quasarsand later, dimmer AGNs. We predict for their Eddington parameter $\lambda_E$ --the ratio of the current to the past black hole accretions -- a bimodaldistribution; the two branches sit now under $\lambda_E \approx 0.01$ (mainlycontributed by low-luminosity AGNs) and around $\lambda_E \approx 0.3-1$. Thesenot only mark out the two populations of AGNs, but also will turn out tocorrelate strongly with the red or blue color of their host galaxies.


Instruction: what is the prompt that generates the input?

Input: The influence of excited-state absorption (ESA) and two-exciton processes ona coherent population transfer with intense ultrashort chirped pulses inmolecular systems in solution has been studied. An unified treatment ofadiabatic rapid passage (ARP) in such systems has been developed using athree-state electronic system with relaxation treated as a diffusion onelectronic potential energy surfaces. We have shown that ESA has a profoundeffect on coherent population transfer in large molecules that necessitates amore accurate interpretation of experimental data. A simple and physicallyclear model for ARP in molecules with three electronic states in solution hasbeen developed by extending the Landau-Zener calculations putting in a thirdlevel to random crossing of levels. A method for quantum control of two-excitonstates in molecular complexes has been proposed.


Instruction: what is the prompt that generates the input?

Input: A combination of experimental techniques and molecular dynamics (MD) computersimulation is used to investigate the diffusion dynamics in Al80Ni20 melts.Experimentally, the self-diffusion coefficient of Ni is measured by thelong-capillary (LC) method and by quasielastic neutron scattering. The LCmethod yields also the interdiffusion coefficient. Whereas the experiments weredone in the normal liquid state, the simulations provided the determination ofboth self-diffusion and interdiffusion constants in the undercooled regime aswell. The simulation results show good agreement with the experimental data. Inthe temperature range 3000 K >= T >= 715 K, the interdiffusion coefficient islarger than the self-diffusion constants. Furthermore the simulation shows thatthis difference becomes larger in the undercooled regime. This result can berefered to a relatively strong temperature dependence of the thermodynamicfactor \Phi, which describes the thermodynamic driving force forinterdiffusion. The simulations also indicate that the Darken equation is agood approximation, even in the undercooled regime. This implies that dynamiccross correlations play a minor role for the temperature range underconsideration.


Instruction: what is the prompt that generates the input?

Input: A characteristic feature of thermalized non-equilibrated matter is that, inspite of energy relaxation--equilibration, a phase memory of the way themany-body system was excited remains. As an example, we analyze data on astrong forward peaking of thermal proton yield in the Bi($\gamma$,p)photonuclear reaction. New analysis shows that the phase relaxation inhighly-excited heavy nuclei can be 8 orders of magnitude or even much longerthan the energy relaxation. We argue that thermalized non-equilibrated matterresembles a high temperature superconducting state in quantum many-bodysystems. We briefly present results on the time-dependent correlation functionof the many-particle density fluctuations for such a superconducting state. Itshould be of interest to experimentally search for manifestations ofthermalized non-equilibrated matter in many-body mesoscopic systems andnanostructures.


Instruction: what is the prompt that generates the input?

Input: The Boltzmann equation for d-dimensional inelastic Maxwell models isconsidered to analyze transport properties in spatially inhomogeneous statesclose to the simple shear flow. A normal solution is obtained via aChapman--Enskog--like expansion around a local shear flow distribution f^{(0)}that retains all the hydrodynamic orders in the shear rate. The constitutiveequations for the heat and momentum fluxes are obtained to first order in thedeviations of the hydrodynamic field gradients from their values in thereference state and the corresponding generalized transport coefficients are{\em exactly} determined in terms of the coefficient of restitution \alpha andthe shear rate a. Since f^{(0)} applies for arbitrary values of the shear rateand is not restricted to weak dissipation, the transport coefficients turn outto be nonlinear functions of both parameters a and \alpha. A comparison withprevious results obtained for inelastic hard spheres from a kinetic model ofthe Boltzmann equation is also carried out.


Instruction: what is the prompt that generates the input?

Input: A recently introduced nonlinear Fokker-Planck equation, derived directly froma master equation, comes out as a very general tool to describephenomenologically systems presenting complex behavior, like anomalousdiffusion, in the presence of external forces. Such an equation ischaracterized by a nonlinear diffusion term that may present, in general, twodistinct powers of the probability distribution. Herein, we calculate thestationary-state distributions of this equation in some special cases, andintroduce associated classes of generalized entropies in order to satisfy theH-theorem. Within this approach, the parameters associated with the transitionrates of the original master-equation are related to such generalizedentropies, and are shown to obey some restrictions. Some particular cases arediscussed.


Instruction: what is the prompt that generates the input?

Input: We have imaged a $\sim$6 arcminute$^2$ region in the Bo\"otes Deep Fieldusing the 350 $\mu$m-optimised second generation Submillimeter High AngularResolution Camera (SHARC II), achieving a peak 1$\sigma$ sensitivity of $\sim$5mJy. We detect three sources above 3$\sigma$, and determine a spurious sourcedetection rate of 1.09 in our maps. In the absence of $5\sigma$ detections, werely on deep 24 $\mu$m and 20 cm imaging to deduce which sources are mostlikely to be genuine, giving two real sources. From this we derive an integralsource count of 0.84$^{+1.39}_{-0.61}$ sources arcmin$^{-2}$ at $S>13$ mJy,which is consistent with 350 $\mu$m source count models that have anIR-luminous galaxy population evolving with redshift. We use these constraintsto consider the future for ground-based short-submillimetre surveys.


Instruction: what is the prompt that generates the input?

Input: The effect of introducing a fifth large-scale space-time dimension to theequations of orbital dynamics was analysed in an earlier paper by the authors.The results showed good agreement with the observed flat rotation curves ofgalaxies and the Pioneer Anomaly. This analysis did not require themodification of Newtonian dynamics, but rather only their restatement in a fivedimensional framework. The same analysis derived a acceleration parameter ar,which plays an important role in the restated equations of orbital dynamics,and suggested a value for ar. In this companion paper, the principle ofconservation of energy is restated within the same five-dimensional framework.The resulting analysis provides an alternative route to estimating the value ofar, without reference to the equations of orbital dynamics, and based solely onkey cosmological constants and parameters, including the gravitationalconstant, G. The same analysis suggests that: (i) the inverse square law ofgravity may itself be due to the conservation of energy at the boundary betweena four-dimensional universe and a fifth large-scale space-time dimension; and(ii) there is a limiting case for the Tulley-Fisher relationship linking thespeed of light to the mass of the Universe.


Instruction: what is the prompt that generates the input?

Input: High-resolution infrared spectroscopy in the 2.3-4.6 micron region isreported for the peculiar A supergiant, single-lined spectroscopic binary HR4049. Lines from the CO fundamental and first overtone, OH fundamental, andseveral H2O vibration-rotation transitions have been observed in thenear-infrared spectrum. The spectrum of HR 4049 appears principally in emissionthrough the 3 and 4.6 micron region and in absorption in the 2 micron region.The 4.6 micron spectrum shows a rich 'forest' of emission lines. All thespectral lines observed in the 2.3-4.6 micron spectrum are shown to becircumbinary in origin. The presence of OH and H2O lines confirm theoxygen-rich nature of the circumbinary gas which is in contrast to thepreviously detected carbon-rich material. The emission and absorption lineprofiles show that the circumbinary gas is located in a thin, rotating layernear the dust disk. The properties of the dust and gas circumbinary disk andthe spectroscopic orbit yield masses for the individual stars, M_AI~0.58 Msolarand M_MV~0.34 Msolar. Gas in the disk also has an outward flow with a velocityof $\gtrsim$ 1 km/s. The severe depletion of refractory elements but near-solarabundances of volatile elements observed in HR 4049 results from abundancewinnowing. The separation of the volatiles from the grains in the disk and thesubsequent accretion by the star are discussed. Contrary to prior reports, theHR 4049 carbon and oxygen isotopic abundances are typical AGB values:12C/13C=6^{+9}_{-4} and 16O/17O>200.


Instruction: what is the prompt that generates the input?

Input: Following deep astrometric and photometric study of the cluster NGC2682(M67), we are able to accurately determine its fundamental parameters. Being anold and rich cluster, M67 is a relevant object for the analysis of the Galacticdisk evolution. M67 is well studied but the lack of a wide and deep Stromgrenphotometric study makes our results worthwhile. The brightest stars of the opencluster M67 were used as uvby-Hbeta standard stars in our studies of NGC1817and NGC2548, and the extension of the field covered, as well as the amount ofobservations, allowed to obtain the best set of Stromgren data ever publishedfor this cluster. We discuss the results of our CCD uvby-Hbetaintermediate-band photometry, covering an area of about 50'x50' down to V 19.Moreover, a complete membership segregation based on astrometric andphotometric criteria is obtained. The photometric analysis of a selected sampleof stars yields a reddening value of E(b-y)= 0.03\pm0.03, a distance modulus ofV_0-M_V= 9.7\pm0.2 and [Fe/H]= 0.01\pm0.14. Through isochrone fitting we foundan age of log t= 9.6\pm0.1 (4.2\pm0.2 Gyr). A clump of approximately 60 starsaround V= 16, (b-y)= 0.4 could be interpreted as a population ofpre-cataclysmic variable stars (if members), or as a stream of field G-typestars placed at twice the distance of the cluster (if non-members).


Instruction: what is the prompt that generates the input?

Input: We employ the Boltzmann equation for describing hadron production from aquark-gluon plasma (QGP) in ultrarelativistic heavy-ion collisions. We proposeresonance formation in quark-antiquark scattering as the dominantmeson-production channel, which, in particular, ensures that energy isconserved in the recombination process. This, in turn, facilitates a morecontrolled extension of hadronization to low transverse momenta ($p_T$), and toaddress the experimentally observed transition from a hydrodynamic regime toconstituent quark-number scaling (CQNS). Based on input distributions forstrange and charm quarks with azimuthal asymmetries, $v_2(p_T)$, characteristicfor RHIC energies, we recover CQNS at sufficiently high $p_T$, while at low$p_T$ a scaling with transverse kinetic energy is found, reminiscent toexperiment. The dependence of the transition regime on microscopic QGPproperties, i.e. resonance widths and $Q$-values in the $q+\bar q \to M$process, is elucidated.


Instruction: what is the prompt that generates the input?

Input: An extension of the Standard Model by three singlet fermions with massessmaller than the electroweak scale allows to explain simultaneously neutrinooscillations, dark matter and baryon asymmetry of the Universe. We discuss theproperties of neutral leptons in this model and the ways they can be searchedfor in particle physics experiments. We establish, in particular, a lower andan upper bound on the strength of interaction of neutral leptons coming fromcosmological considerations and from the data on neutrino oscillations. Weanalyse the production of neutral leptons in the decays of different mesons andin $pp$ collisions. We study in detail decays of neutral leptons and establisha lower bound on their mass coming from existing experimental data and Big BangNucleosynthesis. We argue that the search for a specific missing energy signalin kaon decays would allow to strengthen considerably the bounds on neutralfermion couplings and to find or definitely exclude them below the kaonthreshold. To enter into cosmologically interesting parameter range for massesabove kaon mass the dedicated searches similar to CERN PS191 experiment wouldbe needed with the use of intensive proton beams. We argue that the use ofCNGS, NuMI, T2K or NuTeV beams could allow to search for singlet leptons belowcharm in a large portion of the parameter space of the nuMSM. The search ofsinglet fermions in the mass interval 2-5 GeV would require a considerableincrease of the intensity of proton accelerators or the detailed analysis ofkinematics of more than 10^{10} B-meson decays.


Instruction: what is the prompt that generates the input?

Input: A classical problem in elasticity theory involves an inhomogeneity embeddedin a material of given stress and shear moduli. The inhomogeneity is a regionof arbitrary shape whose stress and shear moduli differ from those of thesurrounding medium. In this paper we present a new, semi-analytic method forfinding the stress tensor for an infinite plate with such an inhomogeneity. Thesolution involves two conformal maps, one from the inside and the second fromthe outside of the unit circle to the inside, and respectively outside, of theinhomogeneity. The method provides a solution by matching the conformal maps onthe boundary between the inhomogeneity and the surrounding material. Thismatching converges well only for relatively mild distortions of the unit circledue to reasons which will be discussed in the article. We provide a comparisonof the present result to known previous results.


Instruction: what is the prompt that generates the input?

Input: An apparatus for producing atomic-gas Bose-Einstein condensates (BECs) of87-Rb atoms is described. The apparatus produces 87-Rb BECs in a dual-chambervacuum system that incorporates magnetic transport of trapped atoms from themagneto-optical trapping cell to the BEC production cell via the operation of aseries of overlapping magnet coils. The design, construction, and operation ofthe apparatus are described in detail. The apparatus is used to study thecreation of quantized vortices in BECs by the merging and interference ofmultiple trapped condensates. In this experiment, a single harmonic potentialwell is partitioned into three sections by an optical barrier, enabling thesimultaneous formation of three independent, uncorrelated BECs. The BECs mayeither merge together during their growth, or, for high-energy barriers, theBECs can be merged together by barrier removal after their formation. Eitherprocess may instigate vortex formation in the resulting BEC, depending on theinitially indeterminate relative phases of the condensates and the mergingrate.


Instruction: what is the prompt that generates the input?

Input: Binary microlensing light curves have a variety of morphologies. Many areindistinguishable from point lens light curves. Of those that deviate from thepoint lens form, caustic crossing light curves have tended to dominateidentified binary lens events. Other distinctive signatures of binary lensesinclude significant asymmetry, multiple peaks, and repeating events. We havequantified, using high resolution simulations, the theoretically expectedrelative numbers of each type of binary lens event, based on its measurablecharacteristics. We find that a microlensing survey with current levels ofphotometric uncertainty and sampling should find at least as many non-causticcrossing binary lens events as caustic crossing events; in future surveys withmore sensitive photometry, the contribution of distinctive non-caustic crossingevents will be even greater. To try to explain why caustic crossing lightcurves appear to be so dominant among the published binary lensing events, weinvestigate the influence of several physical effects, including blending,sampling rate, and various binary populations.


Instruction: what is the prompt that generates the input?

Input: A significant fraction of Lyman Alpha (Lya) emitting galaxies (LAEs) at z>5.7 have rest-frame equivalent widths (EW) greater than ~100 Angstrom. Howeveronly a small fraction of the Lya flux produced by a galaxy is transmittedthrough the IGM, which implies intrinsic Lya EWs that are in excess of themaximum allowed for a population-II stellar population having a Salpeter massfunction. In this paper we study characteristics of the sources powering Lyaemission in high redshift galaxies. We propose a simple model for Lya emittersin which galaxies undergo a burst of very massive star formation that resultsin a large intrinsic EW, followed by a phase of population-II star formationwith a lower EW. We confront this model with a range of high redshiftobservations and find that the model is able to simultaneously describe thefollowing eight properties of the high redshift galaxy population withplausible values for parameters like the efficiency and duration of starformation: i-iv) the UV and Lya luminosity functions of LAEs at z=5.7 and 6.5,v-vi) the mean and variance of the EW distribution of Lya selected galaxies atz=5.7, vii) the EW distribution of i-drop galaxies at z~6, and viii) theobserved correlation of stellar age with EW. Our modeling suggests that theobserved anomalously large intrinsic equivalent widths require a burst of verymassive star formation lasting no more than a few to ten percent of thegalaxies star forming lifetime. This very massive star formation may indicatethe presence of population-III star formation in a few per cent of i-dropgalaxies, and in about half of the Lya selected galaxies.


Instruction: what is the prompt that generates the input?

Input: We present the results from simultaneous chandra and rxte observations of theX-ray bright Broad-Line Radio Galaxy (BLRG) 3C 382. The long (120 ks) exposurewith chandra HETG allows a detailed study of the soft X-ray continuum and ofthe narrow component of the Fe Kalpha line. The rxte PCA data are used to putan upper limit on the broad line component and constrain the hard X-raycontinuum. A strong soft excess below 1 keV is observed in the time-averagedHETG spectrum, which can be parameterized with a steep power law or a thermalmodel. The flux variability at low energies indicates that the origin of thesoft excess cannot be entirely ascribed to the circumnuclear diffuse emission,detected by chandra on scales of 20-30 arcsec (22-33 kpc). A narrow (sigma<90eV) Fe Kalpha line (with EW< 100 eV) is observed by the chandra HEG. Similarvalues for the line parameters are measured by the rxte PCA, suggesting thatthe contribution from a broad line component is negligible. The fact that theexposure is split into two observations taken three days apart allows us toinvestigate the spectral and temporal evolution of the source on differenttimescales. Significant flux variability associated with spectral changes isobserved on timescales of hours and days. The spectral variability is similarto that observed in radio-quiet AGN ruling out a jet-dominated origin of theX-rays.


Instruction: what is the prompt that generates the input?

Input: We review the possibility that the Supersymmetric Standard Model arises fromorbifold constructions of the E_8 x E_8 Heterotic Superstring, and thephenomenological properties that such a model should have. In particular,trying to solve the discrepancy between the unification scale predicted by theHeterotic Superstring (g_{GUT}x5.27x10^{17} GeV) and the value deduced from LEPexperiments (2x10^{16} GeV), we will predict the presence at low energies ofthree families of Higgses and vector-like colour triplets. Our approach relieson the Fayet-Iliopoulos breaking, and this is also a crucial ingredient,together with having three Higgs families, to obtain in these models aninteresting pattern of fermion masses and mixing angles at the renormalizablelebel. Namely, after the gauge breaking some physical particles appear combinedwith other states, and the Yukawa couplings are modified in a well controlledway. On the other hand, dangerous flavour-changing neutral currents may appearwhen fermions of a given charge receive their mass through couplings withseveral Higgs doublets. We will address this potential problem, finding thatviable scenarios can be obtained for a reasonable light Higgs spectrum.


Instruction: what is the prompt that generates the input?

Input: We report the discovery of an X-ray counterpart to the southern radio hotspotof the largest-known radio quasar 4C 74.26 (whose redshift is z=0.104). BothXMM-Newton and Chandra images reveal the same significant (10arcsec, i.e.19kpc) offset between the X-ray hotspot and the radio hotspot imaged withMERLIN. The peak of the X-ray emission may be due to synchrotron orinverse-Compton emission. If synchrotron emission, the hotspot represents thesite of particle acceleration and the offset arises from either the jetexhibiting Scheuer's `dentist's drill' effect or a fast spine having lessmomentum than the sheath surrounding it, which creates the radio hotspot. Ifthe emission arises from the inverse-Compton process, it must beinverse-Compton scattering of the CMB in a decelerating relativistic flow,implying that the jet is relativistic (Gamma >= 2) out to a distance of atleast 800kpc. Our analysis, including optical data from the LiverpoolTelescope, rules out a background AGN for the X-ray emission and confirms itsnature as a hotspot, making it the most X-ray luminous hotspot yet detected.


Instruction: what is the prompt that generates the input?

Input: We introduce and study the notion of relative rigidity for pairs $(X,\JJ)$where 1) $X$ is a hyperbolic metric space and $\JJ$ a collection of quasiconvexsets 2) $X$ is a relatively hyperbolic group and $\JJ$ the collection ofparabolics 3) $X$ is a higher rank symmetric space and $\JJ$ an equivariantcollection of maximal flats Relative rigidity can roughly be described asupgrading a uniformly proper map between two such $\JJ$'s to a quasi-isometrybetween the corresponding $X$'s.  A related notion is that of a $C$-complex which is the adaptation of a Titscomplex to this context. We prove the relative rigidity of the collection ofpairs $(X, \JJ)$ as above. This generalises a result of Schwarz for symmetricpatterns of geodesics in hyperbolic space. We show that a uniformly proper mapinduces an isomorphism of the corresponding $C$-complexes. We also give acouple of characterizations of quasiconvexity. of subgroups of hyperbolicgroups on the way.


Instruction: what is the prompt that generates the input?

Input: This paper quantifies the information rate of multiple-input multiple-output(MIMO) systems with finite rate channel state feedback and power on/offstrategy. In power on/off strategy, a beamforming vector (beam) is eitherturned on (denoted by on-beam) with a constant power or turned off. We provethat the ratio of the optimal number of on-beams and the number of antennasconverges to a constant for a given signal-to-noise ratio (SNR) when the numberof transmit and receive antennas approaches infinity simultaneously and whenbeamforming is perfect. Based on this result, a near optimal strategy, i.e.,power on/off strategy with a constant number of on-beams, is discussed. Forsuch a strategy, we propose the power efficiency factor to quantify the effectof imperfect beamforming. A formula is proposed to compute the maximum powerefficiency factor achievable given a feedback rate. The information rate of theoverall MIMO system can be approximated by combining the asymptotic results andthe formula for power efficiency factor. Simulations show that thisapproximation is accurate for all SNR regimes.


Instruction: what is the prompt that generates the input?

Input: A synfire chain is a simple neural network model which can propagate stablesynchronous spikes called a pulse packet and widely researched. However howsynfire chains coexist in one network remains to be elucidated. We have studiedthe activity of a layered associative network of Leaky Integrate-and-Fireneurons in which connection we embed memory patterns by the Hebbian Learning.We analyzed their activity by the Fokker-Planck method. In our previous report,when a half of neurons belongs to each memory pattern (memory pattern rate$F=0.5$), the temporal profiles of the network activity is split intotemporally clustered groups called sublattices under certain input conditions.In this study, we show that when the network is sparsely connected ($F<0.5$),synchronous firings of the memory pattern are promoted. On the contrary, thedensely connected network ($F>0.5$) inhibit synchronous firings. The sparsenessand denseness also effect the basin of attraction and the storage capacity ofthe embedded memory patterns. We show that the sparsely(densely) connectednetworks enlarge(shrink) the basion of attraction and increase(decrease) thestorage capacity.


Instruction: what is the prompt that generates the input?

Input: We extend previous analyses of the supersymmetric loop correction to theneutral Higgs couplings to include the coupling $\chi^{+}_j \chi^{-}_kH^{0}_l$.The analysis completes the previous analyses where similar corrections werecomputed for the $\bar{\tau} \tau H^{0}_l$, $\bar{b} b H^{0}_l$, $\bar{c} cH^{0}_l$ and for $\bar{t} t H^{0}_l$ couplings within the minimalsupersymmetric standard model. The effective one loop Lagrangian is thenapplied to the computation of the neutral Higgs decays. The sizes of thesupersymmetric loop corrections of the neutral Higgs decay widths into$\chi^{+}_i \chi^{-}_j$ ($i=1,2$; $j=1,2$) are investigated and thesupersymmetric loop correction is found to be in the range of $7\sim15%$ insignificant regions of the parameter space. By including the loop correctionsof the other decay channels $\bar{b} b$, $\bar{t} t$, $\bar{\tau} \tau$,$\bar{c} c$, and $\chi^0_i \chi^0_j$ ($i=1-4$; $j=1-4$), the corrections tobranching ratios for $H^{0}_l\to \chi^{+}_i \chi^{-}_j$ can reach as high as40%.  The effects of CP phases on the branching ratio are also investigated.


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Input: In a number of physically important cases, the nonholonomically(nonintegrable) constrained Ricci flows can be modelled by exact solutions ofEinstein equations with nonhomogeneous (anisotropic) cosmological constants. Wedevelop two geometric methods for constructing such solutions: The firstapproach applies the formalism of nonholonomic frame deformations when thegravitational evolution and field equations transform into systems of nonlinearpartial differential equations which can be integrated in general form. Thesecond approach develops a general scheme when one (two) parameter families ofexact solutions are defined by any source-free solutions of Einstein'sequations with one (two) Killing vector field(s). A successive iterationprocedure results in a class of solutions characterized by an infinite numberof parameters for a non-Abelian group involving arbitrary functions on onevariable. We also consider nonlinear superpositions of some mentioned classesof solutions in order to construct more general integral varieties of the Ricciflow and Einstein equations depending on infinite number of parameters andthree/ four coordinates on four/ five dimensional (semi) Riemannian spaces.


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Input: Many ambitious experiments have been proposed to constrain dark energy anddetect its evolution. At present, observational constraints are consistent witha cosmological constant and there is no firm evidence for any evolution in thedark energy equation of state w. In this paper, we pose the following question:suppose that future dark energy surveys constrain w at low redshift to beconsistent with -1 to a percent level accuracy, what are the implications formodels of dynamical dark energy? We investigate this problem in amodel-independent way by following quintessence field trajectories in `energy'phase-space. Attractor dynamics in this phase-space leads to two classes ofacceptable models: 1) models with flat potentials, i.e. an effectivecosmological constant, and 2) models with potentials that suddenly flatten witha characteristic kink. The prospect of further constraining the second class ofmodels from distance measurements and fluctuation growth rates at low redshift(z<3) seems poor. However, in some models of this second class, the dark energymakes a significant contribution to the total energy density at high redshift.Such models can be further constrained from observation of the cosmic microwavebackground anisotropies and from primordial nucleosynthesis. It is possible,therefore, to construct models in which the dark energy at high redshift causesobservable effects, even if future dark energy surveys constrain w at lowredshift to be consistent with -1 to high precision.


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Input: Since the discovery of the first L dwarf 19 years ago and the discovery ofthe first T dwarf 7 years after that, we have amassed a large list of theseobjects, now numbering almost six hundred. Despite making headway inunderstanding the physical chemistry of their atmospheres, some importantissues remain unexplained. Three of these are the subject of this paper: (1)What is the role of "second parameters" such as gravity and metallicity inshaping the emergent spectra of L and T dwarfs? Can we establish a robustclassification scheme so that objects with unusual values of log(g) or [M/H],unusual dust content, or unresolved binarity are easily recognized? (2) Whichphysical processes drive the unusual behavior at the L/T transition? Whichobservations can be obtained to better confine the problem? (3) What willobjects cooler than T8 look like? How will we know a Y dwarf when we firstobserve one?


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Input: We define Poincar\'e series associated to a toric or analytically irreduciblequasi-ordinary hypersurface singularity, (S,0), by a finite sequence ofmonomial valuations, such that at least one of them is centered at the origin0. This involves the definition of a multi-graded ring associated to theanalytic algebra of the singularity by the sequence of valuations. We provethat the Poincar\'e series is a rational function with integer coefficients,which can be defined also as an integral with respect of the Eulercharacteristic, over the projectivization of the analytic algebra of thesingularity, of a function defined by the valuations. In particular, thePoincar\'e series associated to the set of divisorial valuations associated tothe essential divisors, considered both over the singular locus and over thepoint 0, is an analytic invariant of the singularity. In the quasi-ordinaryhypersurface case we prove that this Poincar\'e series determines and it isdetermined by the normalized sequence of characteristic monomials. Thesemonomials in the analytic case define a complete invariant of the embeddedtopological type of the hypersurface singularity.


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Input: We present analytical and numerical studies of phase-coherent dynamics ofintrinsically localized excitations (breathers) in a system of two weaklycoupled nonlinear oscillator chains. We show that there are two qualitativelydifferent dynamical regimes of the coupled breathers, either immovable orslowly-moving: the periodic transverse translation (wandering) of low-amplitudebreather between the chains, and the one-chain-localization of high-amplitudebreather. These two modes of coupled nonlinear excitations, which involve largenumber of anharmonic oscillators, can be mapped onto two solutions of a singlependulum equation, detached by a separatrix mode. We also study two-chainbreathers, which can be considered as bound states of discrete breathers withdifferent symmetry and center locations in the coupled chains, and bifurcationof the anti-phase two-chain breather into the one-chain one. Delocalizingtransition of 1D breather in 2D system of a large number of parallel couplednonlinear chains is described, in which the breather, initially excited in agiven chain, abruptly spreads its vibration energy in the whole 2D system upondecreasing breather frequency or amplitude below the threshold one. Thethreshold breather frequency is above the cut off phonon frequency in 2Dsystem, and the threshold breather amplitude scales as square root of theinter-chain coupling constant. Delocalizing transition of discrete vibrationalbreather in 2D and 3D systems of coupled nonlinear chains has an analogy withdelocalizing transition for Bose-Einstein condensates in 2D and 3D opticallattices.


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Input: The vacuum dependence on boundary conditions in quantum field theories isanalysed from a very general viewpoint. From this perspective therenormalization prescriptions not only imply the renormalization of thecouplings of the theory in the bulk but also the appearance of a flow in thespace of boundary conditions. For regular boundaries this flow has a largevariety of fixed points and no cyclic orbit. The family of fixed pointsincludes Neumann and Dirichlet boundary conditions. In one-dimensional fieldtheories pseudoperiodic and quasiperiodic boundary conditions are also RG fixedpoints. Under these conditions massless bosonic free field theories areconformally invariant. Among all fixed points only Neumann boundary conditionsare infrared stable fixed points. All other conformal invariant boundaryconditions become unstable under some relevant perturbations. In finite volumeswe analyse the dependence of the vacuum energy along the trajectories of therenormalization group flow providing an interesting framework for dark energyevolution. On the contrary, the renormalization group flow on the boundary doesnot affect the leading behaviour of the entanglement entropy of the vacuum inone-dimensional conformally invariant bosonic theories.


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Input: In this paper, it is shown that the cosmological model that was introduced ina sequence of three earlier papers under the title, A Dust Universe Solution tothe Dark Energy Problem, can be used to resolve the problem of the greatmismatch of numerical values between dark energy from cosmology and zero pointenergy from quantum theory. It is shown that, if the zero point energies forthe cosmic microwave background and for all the rest of the universe that isnot cosmic microwave background are introduced into this model as two entities,their separate values appear within this theory in the form of a numericaldifference. It is this difference that gives the numerical value for the zeropoint value of Einstein's dark energy density. Consequently, although the twozero point energies may be large, their difference can give the known smalldark energy value from cosmology for dark energy density. Issues relating tointerpretation, calculation and measurement associated with this result and aninterpretation of dark energy as a measure of polarisation of the vacuum arediscussed. In the first appendix to this paper, problems associated with thestandard model of cosmology are solved by redefining temperature in the dustuniverse model. In the second appendix of this paper, an examination of thedark matter problem in relation to a general relativistic generalisation ofNewton's inverse square law is undertaken. In the third appendix to this paper,the formalism is used to derive a formula that gives a possible value for themass of the universe in terms of Newton's gravitation constant, Einstein'sLambda and the velocity of light. All three appendices have their own detailedabstracts.


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Input: By analyzing the relationships between a socioeconomical system modeledthrough evolutionary game theory and a physical system modeled through quantummechanics we show how although both systems are described through two theoriesapparently different both are analogous and thus exactly equivalents. Theextensions of quantum mechanics to statistical physics and information theorylet us use some of their definitions for the best understanding of the behaviorof economics and biology. The quantum analogue of the replicator dynamics isthe von Neumann equation. A system in where all its members are in Nashequilibrium is equivalent to a system in a maximum entropy state. Nature is agame in where its players compete for a common welfare and the equilibrium ofthe system that they are members. They act as a whole besides individuals likethey obey a rule in where they prefer to work for the welfare of the collectivebesides the individual welfare.


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Input: The calculation of conserved charges of black holes is a rich problem, forwhich many methods are known. Until recently, there was some controversy on theproper definition of conserved charges in asymptotically anti-de Sitter (AdS)spaces in arbitrary dimensions. This paper provides a systematic and explicitHamiltonian derivation of the energy and the angular momenta of bothasymptotically flat and asymptotically AdS spacetimes in any dimension D biggeror equal to 4. This requires as a first step a precise determination of theasymptotic conditions of the metric and of its conjugate momentum. Theseconditions happen to be achieved in ellipsoidal coordinates adapted to therotating solutions.The asymptotic symmetry algebra is found to be isomorphiceither to the Poincare algebra or to the so(D-1, 2) algebra, as expected. Inthe asymptotically flat case, the boundary conditions involve a generalizationof the parity conditions, introduced by Regge and Teitelboim, which arenecessary to make the angular momenta finite. The charges are explicitlycomputed for Kerr and Kerr-AdS black holes for arbitrary D and they are shownto be in agreement with thermodynamical arguments.


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Input: We report the discovery of one of the most powerful sunquakes detected todate, produced by an X1.2-class solar flare in active region 10720 on 2005January 15. We used helioseismic holography to image the source of seismicwaves emitted into the solar interior from the site of the flare. Acousticegression power maps at 3 and 6 mHz with a 2 mHz bandpass reveal a compactacoustic source strongly correlated with impulsive hard X-ray andvisible-continuum emission along the penumbral neutral line separating the twomajor opposing umbrae in the $\delta$-configuration sunspot that predominatesAR10720. The acoustic emission signatures were directly aligned with both hardX-ray and visible continuum emission that emanated during the flare. Thevisible continuum emission is estimated at $2.0 \times 10^{23}$ J,approximately 500 times the seismic emission of $\sim 4 \times 10^{20}$ J. Theflare of 2005 January 15 exhibits the same close spatial alignment between thesources of the seismic emission and impulsive visible continuum emission asprevious flares, reinforcing the hypothesis that the acoustic emission may bedriven by heating of the low photosphere. However, it is a major exception inthat there was no signature to indicate the inclusion of protons in theparticle beams thought to supply the energy radiated by the flare. Thecontinued strong coincidence between the sources of seismic emission andimpulsive visible continuum emission in the case of a proton-deficientwhite-light flare lends substantial support to the ``back -- warming''hypothesis, that the low photosphere is significantly heated by intense Balmerand Paschen continuum-edge radiation from the overlying chromosphere inwhite-light flares.


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Input: We construct a commutative algebra A_x of difference operators in R^p,depending on p+3 real parameters which is diagonalized by the multivariableRacah polynomials R_p(n;x) considered by Tratnik [27]. It is shown that forspecific values of the variables x=(x_1,x_2,...,x_p) there is a hidden dualitybetween n and x. Analytic continuation allows us to construct anothercommutative algebra A_n in the variables n=(n_1,n_2,...,n_p) which is alsodiagonalized by R_p(n;x). Thus R_p(n;x) solve a multivariable discretebispectral problem in the sense of Duistermaat and Grunbaum [8]. Since a changeof the variables and the parameters in the Racah polynomials gives themultivariable Wilson polynomials [26], this change of variables and parametersin A_x and A_n leads to bispectral commutative algebras for the multivariableWilson polynomials.


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Input: A recent advance in improving the spatial resolution of magnetic forcemicroscopy (MFM) uses as sensor tips carbon nanotubes grown at the apex ofconventional silicon cantilever pyramids and coated with a thin ferromagneticlayer. Magnetic images of high density vertically recorded media using thesetips exhibit a doubling of the spatial frequency under some conditions. Here wedemonstrate that this spatial frequency doubling is due to the switching of themoment direction of the nanotube tip. This results in a signal which isproportional to the absolute value of the signal normally observed in MFM. Ourmodeling indicates that a significant fraction of the tip volume is involved inthe observed switching, and that it should be possible to image very high bitdensities with nanotube magnetic force sensors.


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Input: We consider normalizers of an irreducible inclusion $N\subseteq M$ of$\mathrm{II}_1$ factors. In the infinite index setting an inclusion$uNu^*\subseteq N$ can be strict, forcing us to also investigate the semigroupof one-sided normalizers. We relate these normalizers of $N$ in $M$ toprojections in the basic construction and show that every trace one projectionin the relative commutant $N'\cap < M,e_N>$ is of the form $u^*e_Nu$ for someunitary $u\in M$ with $uNu^*\subseteq N$. This enables us to identify thenormalizers and the algebras they generate in several situations. In particulareach normalizer of a tensor product of irreducible subfactors is a tensorproduct of normalizers modulo a unitary. We also examine normalizers ofirreducible subfactors arising from subgroup--group inclusions $H\subseteq G$.Here the normalizers are the normalizing group elements modulo a unitary from$L(H)$. We are also able to identify the finite trace $L(H)$-bimodules in$\ell^2(G)$ as double cosets which are also finite unions of left cosets.


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Input: We derive the microcanonical partition function of the ideal relativisticquantum gas of spinless bosons in a quantum field framework as an expansionover fixed multiplicities. Our calculation generalizes well known expressionsin literature in that it does not introduce any large volume approximation andit is valid at any volume. We discuss the issues concerned with the definitionof the microcanonical ensemble for a free quantum field at volumes comparablewith the Compton wavelength and provide a consistent prescription ofcalculating the microcanonical partition function, which is finite at finitevolume and yielding the correct thermodynamic limit. Besides an immaterialoverall factor, the obtained expression turns out to be the same as in thenon-relativistic multi-particle approach. This work is introductory to derivethe most general expression of the microcanonical partition function fixing themaximal set of observables of the Poincare' group.


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Input: Colliding winds of massive stars in binary systems are considered ascandidate sites of high-energy non-thermal photon emission. They are alreadyamong the suggested counterparts for a few individual unidentified EGRETsources, but may constitute a detectable source population for the GLASTobservatory. The present work investigates such population study of massivecolliding wind systems at high-energy gamma-rays. Based on the recent detailedmodel (Reimer et al. 2006) for non-thermal photon production in prime candidatesystems, we unveil the expected characteristics of this source class in theobservables accessible at LAT energies. Combining the broadband emission modelwith the presently cataloged distribution of such systems and their individualparameters allows us to conclude on the expected maximum number ofLAT-detections among massive stars in colliding wind binary systems.


Instruction: what is the prompt that generates the input?

Input: We examine Gaussian-basis Monte Carlo method (GBMC) introduced by Corney andDrummond. This method is based on an expansion of the density-matrix operatorrho by means of the coherent Gaussian-type operator basis Lambda and does notsuffer from the minus sign problem. The original method, however, often failsin reproducing the true ground state and causes systematic errors of calculatedphysical quantities because the samples are often trapped in some metastable orsymmetry broken states. To overcome this difficulty, we combine thequantum-number projection scheme proposed by Assaad, Werner, Corboz, Gull andTroyer in conjunction with the importance sampling of the original GBMC method.This improvement allows us to carry out the importance sampling in thequantum-number-projected phase-space. Some comparisons with the previousquantum-number projection scheme indicate that, in our method, the convergencewith the ground state is accelerated, which makes it possible to extend theapplicability and widen the range of tractable parameters in the GBMC method.The present scheme offers an efficient practical way of computation forstrongly correlated electron systems beyond the range of system sizes,interaction strengths and lattice structures tractable by other computationalmethods such as the quantum Monte Carlo method.


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Input: Hundreds of substellar companions to solar-type stars will be discovered withthe Kepler satellite. Kepler's extreme photometric precision gives access tolow-amplitude stellar variability contributed by a variety of physicalprocesses. We discuss in detail the periodic flux modulations arising from thetidal force on the star due to a substellar companion. An analytic expressionfor the variability is derived in the equilibrium-tide approximation. Wedemonstrate analytically and through numerical solutions of the linear,nonadiabatic stellar oscillation equations that the equilibrium-tide formulaworks extremely well for stars of mass <1.4 Msun with thick surface convectionzones. More massive stars with largely radiative envelopes do not conform tothe equilibrium-tide approximation and can exhibit flux variations $\ga$10times larger than naive estimates. Over the full range of stellar massesconsidered, we treat the oscillatory response of the convection zone byadapting a prescription that A. J. Brickhill developed for pulsating whitedwarfs. Compared to other sources of periodic variability, the ellipsoidallightcurve has a distinct dependence on time and system parameters. We suggestthat ellipsoidal oscillations induced by giant planets may be detectable fromas many as ~100 of the 10^5 Kepler target stars. (Abridged)


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Input: In papers I and II in this series, we presented hydrodynamical simulations ofjet models with parameters representative of the symbiotic system MWC 560.These were simulations of a pulsed, initially underdense jet in a high densityambient medium. Since the pulsed emission of the jet creates internal shocksand since the jet velocity is very high, the jet bow shock and the internalshocks are heated to high temperatures and should therefore emit X-rayradiation. In this paper, we investigate in detail the X-ray properties of thejets in our models. We have focused our study on the total X-ray luminosity andits temporal variability, the resulting spectra and the spatial distribution ofthe emission. Temperature and density maps from our hydrodynamical simulationswith radiative cooling presented in the second paper are used together withemissivities calculated with the atomic database ATOMDB. The jets in our modelsshow extended and variable X-ray emission which can be characterized as a sumof hot and warm components with temperatures that are consistent withobservations of CH Cyg and R Aqr. The X-ray spectra of our model jets showemission line features which correspond to observed features in the spectra ofCH Cyg. The innermost parts of our pulsed jets show iron line emission in the6.4 - 6.7 keV range which may explain such emission from the central source inR Aqr. We conclude that MWC 560 should be detectable with Chandra orXMM-Newton, and such X-ray observations will provide crucial for understandingjets in symbiotic stars.


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Input: We study theoretically the Josephson effect in d-wave superconductor /diffusive normal metal /insulator/ diffusive normal metal/ d-wavesuperconductor (D/DN/I/DN/D) junctions. This model is aimed to describepractical junctions in high-$T_C$ cuprate superconductors, in which the productof the critical Josephson current ($I_C$) and the normal state resistance ($R$)(the so-called $I_{\rm C}R$ product) is very small compared to the predictionof the standard theory. We show that the $I_{\rm C}R$ product in D/DN/I/DN/Djunctions can be much smaller than that in d-wave superconductor / insulator /d-wave superconductor junctions and formulate the conditions necessary toachieve large $I_{\rm C}R$ product in D/DN/I/DN/D junctions. The proposedtheory describes the behavior of $I_{\rm C}R$ products quantitatively inhigh-$T_{\rm C}$ cuprate junctions.


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Input: The object NGC6908 was once thought to be simply a surface-brightnessenhancement in the eastern spiral arm of the nearby spiral galaxy NGC6907.Based on an examination of near-infrared imaging, the object is shown in factto be a lenticular S0(6/7) galaxy hidden in the optical glare of the disk andspiral structure of the larger galaxy. New radial velocities of NGC6908(3,060+/-16 (emission); 3,113+/-73 km/s (absorption)) have been obtained at theBaade 6.5m and the duPont 2.5m telescopes at Las Campanas, Chile placingNGC6908 at the same expansion-velocity distance as NGC6907 (3,190+/-5 km/s),eliminating the possibility of a purely chance line-of-sight coincidence. Theonce-enigmatic asymmetries in the disk and outer spiral structure of NGC6907are now explained as being due to an advanced merger event. Newly discoveredtails and debris in the outer reaches of this galaxy further support the mergerscenario for this system. This pair of galaxies is a rather striking example oftwo objects discovered over 100 years ago, whose true nature was lost untilmodern detectors operating at infrared wavelengths gave us a new(high-contrast) look. Other examples of embedded merger remnants may alsoreveal themselves in the growing samples of near-infrared imaging of nearbygalaxies; and a pilot study does reveal several other promising candidates forfollow-up observations.


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Input: GEMS and GOODS fields were examined to z~1.4 for galaxy interactions andmergers. The basic morphologies are familiar: antennae with long tidal tails,tidal dwarfs, and merged cores; M51-type galaxies with disk spirals and tidalarm companions; early-type galaxies with diffuse plumes; equal-massgrazing-collisions; and thick J-shaped tails beaded with star formation anddouble cores. One type is not common locally and is apparently a looseassemblage of smaller galaxies. Photometric measurements were made of the tailsand clumps, and physical sizes were determined assuming photometric redshifts.Antennae tails are a factor of ~3 smaller in GEMS and GOODS systems compared tolocal antennae; their disks are a factor of ~2 smaller than locally. Collisionsamong early type galaxies generally show no fine structure in their tails,indicating that stellar debris is usually not unstable. One exception has a5x10**9 Msun smooth red clump that could be a pure stellar condensation. Mosttidal dwarfs are blue and probably form by gravitational instabilities in thegas. One tidal dwarf looks like it existed previously and was incorporated intothe arm tip by tidal forces. The star-forming regions in tidal arms are 10 to1000 times more massive than star complexes in local galaxies, although theirseparations are about the same. If they all form by gravitationalinstabilities, then the gaseous velocity dispersions in interacting galaxieshave to be larger than in local galaxies by a factor of ~5 or more; the gascolumn densities have to be larger by the square of this factor.


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Input: We present the fourth edition of the Sloan Digital Sky Survey (SDSS) QuasarCatalog. The catalog contains 77,429 objects; this is an increase of over30,000 entries since the previous edition. The catalog consists of the objectsin the SDSS Fifth Data Release that have luminosities larger than M_i = -22.0(in a cosmology with H_0 = 70 km/s/Mpc, Omega_M = 0.3, and Omega_Lambda = 0.7)have at least one emission line with FWHM larger than 1000 km/s, or haveinteresting/complex absorption features, are fainter than i=15.0, and havehighly reliable redshifts. The area covered by the catalog is 5740 sq. deg. Thequasar redshifts range from 0.08 to 5.41, with a median value of 1.48; thecatalog includes 891 quasars at redshifts greater than four, of which 36 are atredshifts greater than five. Approximately half of the catalog quasars have i <19; nearly all have i < 21. For each object the catalog presents positionsaccurate to better than 0.2 arcsec. rms per coordinate, five-band (ugriz)CCD-based photometry with typical accuracy of 0.03 mag, and information on themorphology and selection method. The catalog also contains basic radio,near-infrared, and X-ray emission properties of the quasars, when available,from other large-area surveys. The calibrated digital spectra cover thewavelength region 3800--9200A at a spectral resolution of ~2000. The spectracan be retrieved from the public database using the information provided in thecatalog. The average SDSS colors of quasars as a function of redshift, derivedfrom the catalog entries, are presented in tabular form. Approximately 96% ofthe objects in the catalog were discovered by the SDSS.


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Input: We study to what extent wormholes can mimic the observational features ofblack holes. It is surprisingly found that many features that could be thoughtof as ``characteristic'' of a black hole (endowed with an event horizon) can beclosely mimicked by a globally static wormhole, having no event horizon. Thisis the case for: the apparently irreversible accretion of matter down a hole,no-hair properties, quasi-normal-mode ringing, and even the dissipativeproperties of black hole horizons, such as a finite surface resistivity equalto 377 Ohms. The only way to distinguish the two geometries on anobservationally reasonable time scale would be through the detection ofHawking's radiation, which is, however, too weak to be of practical relevancefor astrophysical black holes. We point out the existence of an interestingspectrum of quantum microstates trapped in the throat of a wormhole which couldbe relevant for storing the information ``lost'' during a gravitationalcollapse.


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Input: The network of resonant bar detectors of gravitational waves resumedcoordinated observations within the International Gravitational EventCollaboration (IGEC-2). Four detectors are taking part in this collaboration:ALLEGRO, AURIGA, EXPLORER and NAUTILUS. We present here the results of thesearch for gravitational wave bursts over 6 months during 2005, when IGEC-2 wasthe only gravitational wave observatory in operation. The network data analysisimplemented is based on a time coincidence search among AURIGA, EXPLORER andNAUTILUS, keeping the data from ALLEGRO for follow-up studies. With respect tothe previous IGEC 1997-2000 observations, the amplitude sensitivity of thedetectors to bursts improved by a factor about 3 and the sensitivity bandwidthsare wider, so that the data analysis was tuned considering a larger class ofdetectable waveforms. Thanks to the higher duty cycles of the single detectors,we decided to focus the analysis on three-fold observation, so to ensure theidentification of any single candidate of gravitational waves (gw) with highstatistical confidence. The achieved false detection rate is as low as 1 percentury. No candidates were found.


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Input: High resolution molecular line observations of CS, HCO+, C18O and N2H+ wereobtained toward the starless globule FeSt 1-457 in order to investigate itskinematics and chemistry. The HCO+ and CS spectra show clear self-reversed andasymmetric profiles across the face of the globule. The sense of the observedasymmetry is indicative of the global presence of expansion motions in theouter layers of the globule. These motions appear to be subsonic andsignificantly below the escape velocity of the globule. Comparison of ourobservations with near-infrared extinction data indicate that the globule isgravitationally bound. Taken together these considerations lead us to suggestthat the observed expansion has its origin in an oscillatory motion of theouter layers of the globule which itself is likely in a quasi-stable state nearhydrostatic equilibrium. Analysis of the observed linewidths of CO and N2H+confirm that thermal pressure is the dominant component of the cloud's internalsupport. A simple calculation suggests that the dominant mode of pulsationwould be an l = 2 mode with a period of 0.3 Myr. Deformation of the globule dueto the large amplitude l = 2 oscillation may be responsible for thedouble-peaked structure of the core detected in high resolution extinctionmaps. Detailed comparison of the molecular-line observations and extinctiondata provides evidence for significant depletion of C18O and perhaps HCO+ whileN2H+ may be undepleted to a cloud depth of about 40 magnitudes of visualextinction.


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Input: Ordinal regression is an important type of learning, which has properties ofboth classification and regression. Here we describe a simple and effectiveapproach to adapt a traditional neural network to learn ordinal categories. Ourapproach is a generalization of the perceptron method for ordinal regression.On several benchmark datasets, our method (NNRank) outperforms a neural networkclassification method. Compared with the ordinal regression methods usingGaussian processes and support vector machines, NNRank achieves comparableperformance. Moreover, NNRank has the advantages of traditional neuralnetworks: learning in both online and batch modes, handling very large trainingdatasets, and making rapid predictions. These features make NNRank a useful andcomplementary tool for large-scale data processing tasks such as informationretrieval, web page ranking, collaborative filtering, and protein ranking inBioinformatics.


Instruction: what is the prompt that generates the input?

Input: In this article, we report the synthesis, magneto transport features, andmagnetization of polycrystalline La2/3Ca1/3MnO3:Agx/Inx composites with x = 0,0.1, 0.2, 0.3 and 0.4. In case of Ag the temperature coefficient of resistance(TCR) near ferromagnetic (FM) transition enhances significantly with additionof Ag. The FM transition temperature (TFM) is also increased slightly with Agdoping. Magneto-transport measurements revealed that magneto-resistance (MR) isfound to be maximum near TFM. Very sharp TCR is seen near TFM with highestvalue of up to 15 % for Ag (0.4) sample, which is an order of magnitude higherthan as for pristine sample and is the best value yet reported for anypolycrystalline LCMO compound. Increased TCR, TFM and significant above roomtemperature MR of La2/3Ca1/3MnO3:Agx composites is explained on the basis ofimproved grains size. Interestingly the La2/3Ca1/3MnO3:Inx composites behavedexactly in opposite way resulting in decreased TFM, and TCR compared topristine LCMO compound. In fact the grains morphology of LCMO:Inx composites isseen inferior to pristine LCMO which is opposite to the LCMO:Agx case.


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Input: We calculate angle-resolved above-threshold ionization spectra for diatomicmolecules in linearly polarized laser fields, employing the strong-fieldapproximation. The interference structure resulting from the individualcontributions of the different scattering scenarios is discussed in detail,with respect to the dependence on the internuclear distance and molecularorientation. We show that, in general, the contributions from the processes inwhich the electron is freed at one center and rescatters off the other obscurethe interference maxima and minima obtained from single-center processes.However, around the boundary of the energy regions for which rescattering has aclassical counterpart, such processes play a negligible role and very clearinterference patterns are observed. In such energy regions, one is able toinfer the internuclear distance from the energy difference between adjacentinterference minima.


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Input: We discuss Casimir effect of a massless, minimally coupled scalar field in a6D warped flux compactification model and its implications for the hierarchyand cosmological constant problems, which are longstanding puzzles inphenomenology and cosmology. Due to the scale invariance of the backgroundtheory, the 4D effective theory contains a volume modulus. To stabilize themodulus, we consider one-loop corrections to the effective potential by theCasimir effect. The one-loop effective potential for the volume modulus has aform which is very similar to Coleman-Weinberg potential. We evaluatecoefficients appearing in the effective potential by employing zeta functionregularization and heat kernel analysis. The volume modulus is stabilized forsmaller degrees of warping, below a critical value, which depends on deficitangle of the reference brane. After stabilizing the modulus, it is possible toobtain observed values of the mass ratio between the fundamental energy scalesand a tiny effective cosmological constant (though its sign is negative). Thedegree of warping should be tuned to be close to the critical value, not asseverely as the original fine-tuning.


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Input: The critical behavior of the contact process in disordered and periodicbinary 2d-lattices is investigated numerically by means of Monte Carlosimulations as well as via an analytical approximation and standard mean fieldtheory. Phase-separation lines calculated numerically are found to agree wellwith analytical predictions around the homogeneous point. For the disorderedcase, values of static scaling exponents obtained via quasi-stationarysimulations are found to change with disorder strength. In particular, thefinite-size scaling exponent of the density of infected sites approaches avalue consistent with the existence of an infinite-randomness fixed point asconjectured before for the 2d disordered CP. At the same time, both dynamicaland static scaling exponents are found to coincide with the values establishedfor the homogeneous case thus confirming that the contact process in aheterogeneous environment belongs to the directed percolation universalityclass.


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Input: We recently proposed an empirical approach for the Landau-Pomeranchuk-Migdal(LPM) effects in photon emission from the quark gluon plasma as a function ofphoton mass. This approach was based on Generalized Emission Functions (GEF)for photon emission, derived at a fixed temperature and strong couplingconstant. In the present work, we have extended the LPM calculations forseveral temperatures and strong coupling strengths. The integral equations for(${\bf \tilde{f}(\tilde{p}_\perp)}$) and ($\tilde{g}({\bf \tilde{p}_\perp})$)are solved by the iterations method for the variable set\{$p_0,q_0,Q^2,T,\alpha_s$\}, considering bremsstrahlung and $\bf aws$processes. We generalize the dynamical scaling variables, $x_T$, $x_L$, forbremsstrahlung and {\bf aws} processes which are now functions of variables$p_0,q_0,Q^2,T,\alpha_s$. The GEF introduced earlier, $g^b_T$, $g^a_T$,$g^b_L$, $g^a_L$, are also generalized for any temperatures and couplingstrengths. From this, the imaginary part of the photon polarization tensor as afunction of photon mass and energy can be calculated as a one dimensionalintegral over these GEF and parton distribution functions in the plasma.However, for phenomenological studies of experimental data, one needs a simpleempirical formula without involving parton momentum integrations. Therefore, wepresent a phenomenological formula for imaginary photon polarization tensor asa function of \{$q_0,Q^2,T,\alpha_s$\} that includes bremsstrahlung and $\bfaws$ mechanisms along with LPM effects.


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Input: Disordered systems present multifractal properties at criticality. Inparticular, as discovered by Ludwig (A.W.W. Ludwig, Nucl. Phys. B 330, 639(1990)) on the case of diluted two-dimensional Potts model, the moments$\bar{\rho^q(r)}$ of the local order parameter $\rho(r)$ scale with a set$x(q)$ of non-trivial exponents $x(q) \neq q x(1)$. In this paper, we revisitthese ideas to incorporate more recent findings: (i) whenever a multifractalmeasure $w(r)$ normalized over space $ \sum_r w(r)=1$ occurs in a randomsystem, it is crucial to distinguish between the typical values and thedisorder averaged values of the generalized moments $Y_q =\sum_r w^q(r)$, sincethey may scale with different generalized dimensions $D(q)$ and $\tilde D(q)$(ii) as discovered by Wiseman and Domany (S. Wiseman and E. Domany, Phys Rev E{\bf 52}, 3469 (1995)), the presence of an infinite correlation length inducesa lack of self-averaging at critical points for thermodynamic observables, inparticular for the order parameter. After this general discussion valid for anyrandom critical point, we apply these ideas to random polymer models that canbe studied numerically for large sizes and good statistics over the samples. Westudy the bidimensional wetting or the Poland-Scheraga DNA model with loopexponent $c=1.5$ (marginal disorder) and $c=1.75$ (relevant disorder). Finally,we argue that the presence of finite Griffiths ordered clusters at criticalitydetermines the asymptotic value $x(q \to \infty) =d$ and the minimal value $\alpha_{min}=D(q \to \infty)=d-x(1) $ of the typical multifractal spectrum$f(\alpha)$.


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Input: This thesis provides a partial answer to a question posed by Greg Kuperbergin q-alg/9712003 and again by Justin Roberts as problem 12.18 in "Problems oninvariants of knots and 3-manifolds", math.GT/0406190, essentially: "Can onedescribe the category of representations of the quantum group U_q(sl_n)(thought of as a spherical category) via generators and relations?"  For each n \geq 0, I define a certain tensor category of trivalent graphs,modulo isotopy, and construct a functor from this category onto (a fullsubcategory of) the category of representations of the quantum group U_q(sl_n).One would like to describe completely the kernel of this functor, by providinggenerators. The resulting quotient of the diagrammatic category would then be acategory equivalent to the representation category of U_q(sl_n).  I make significant progress towards this, describing certain generators ofthe kernel, and some obstructions to further elements. It remains a conjecturethat these relations generate the kernel. My results extend those ofq-alg/9712003, MR1659228, math.QA/0310143 and math.GT/0506403.  The argument is essentially by constructing a diagrammatic version of theforgetful functor coming from the inclusion of U_q(sl_{n-1}) in U_q(sl_n}. Weknow this functor is faithful, so a diagram is in the kernel for n exactly ifits image under the diagrammatic forgetful functor is in the kernel for n-1.This allows us to perform inductive calculations, both establishing families ofelements of the kernel, and finding obstructions.


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Input: In this article we calculate the surface phase diagram of a two-dimensionalhard-rod fluid confined between two hard lines. In a first stage we study thesemi-infinite system consisting of an isotropic fluid in contact with a singlehard line. We have found complete wetting by the columnar phase at thewall-isotropic fluid interface. When the fluid is confined between two hardwalls, capillary columnar ordering occurs via a first-order phase transition.For higher chemical potentials the system exhibits layering transitions evenfor very narrow slits (near the one-dimensional limit). The theoretical modelused was a density-functional theory based on the Fundamental-MeasureFunctional applied to a fluid of hard rectangles in the restricted-orientationapproximation (Zwanzig model). The results presented here can be checkedexperimentally in two-dimensional granular media made of rods, where verticalmotions induced by an external source and excluded volume interactions betweenthe grains allow the system to explore those stationary states whichentropically maximize packing configurations. We claim that some of the surfacephenomena found here can be present in two-dimensional granular-media fluids.


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Input: We present an examination of the kinematics and stellar populations of asample of 3 Brightest Group Galaxies (BGGs) and 3 Brightest Cluster Galaxies(BCGs) in X-ray groups and clusters. We have obtained high signal-to-noiseGemini/GMOS (Gemini South Multi-Object Spectrograph) long-slit spectra of thesegalaxies and use Lick indices to determine ages, metallicities andalpha-element abundance ratios out to at least their effective radii. We findthat the BGGs and BCGs have very uniform masses, central ages and centralmetallicities. Examining the radial dependence of their stellar populations, wefind no significant velocity dispersion, age, or alpha-enhancement gradients.However, we find a wide range of metallicity gradients, suggesting a variety offormation mechanisms. The range of metallicity gradients observed is surprisinggiven the homogeneous environment these galaxies probe and their uniformcentral stellar populations. However, our results are inconsistent with anysingle model of galaxy formation and emphasize the need for more theoreticalunderstanding of both the origins of metallicity gradients and galaxy formationitself. We postulate two possible physical causes for the different formationmechanisms.


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Input: We present the first result of the Ital-FLAMES survey of red giant branch(RGB) stars in omega Cen. Radial velocities with a precision of ~0.5 km/s arepresented for 650 members of omega Cen observed with FLAMES-Giraffe at the VeryLarge Telescope. We found that stars belonging to the metal -poor (RGB-MP),metal-intemediate (RGB-MInt) and metal-rich (RGB-a) sub -populations of OmegaCen are all compatible with having the same rotational pattern. Our resultsappear to contradict past findings by Norris et al., who could not detect anyrotational signature for metal -rich stars. The slightly higher precision ofthe present measurements and the much larger sample size, especially for themetal-richer stars, appear as the most likely explanation for this discrepancy.The result presented here weakens the body of evidence in favour of a mergerevent in the past history of omega Cen.


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Input: This is the second of two papers reporting observations and analysis of theunusually bright (m_b=14.4), luminous (M_B=-25.5), nearby (z=0.192) narrow-linequasar PHL 1811. The first paper reported that PHL 1811 is intrinsically X-rayweak, and presented a spectral energy distribution (SED). Here we present HSTSTIS optical and UV spectra, and ground-based optical spectra. The optical andUV line emission is very unusual. There is no evidence for forbidden orsemiforbidden lines. The near-UV spectrum is dominated by very strong FeII andFeIII, and unusual low-ionization lines such as NaID and CaII H&K are observed.High-ionization lines are very weak; CIV has an equivalent width of 6.6A, afactor of ~5 smaller than measured from quasar composite spectra. An unusualfeature near 1200A can be deblended in terms of Ly\alpha, NV, SiII, and CIII*using the blueshifted CIV profile as a template. Photoionization modeling showsthat the unusual line emission can be explained qualitatively by the unusuallysoft SED. Principally, a low gas temperature results in inefficient emission ofcollisionally excited lines, including the semiforbidden lines generally usedas density diagnostics. The emission resembles that of high-density gas; inboth cases this is a consequence of inefficient cooling. PHL 1811 is veryunusual, but we note that quasar surveys are generally biased against findingsimilar objects.


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Input: The science of complex networks is a new interdisciplinary branch of sciencewhich has arisen recently on the interface of physics, biology, social andcomputer sciences, and others. Its main goal is to discover general lawsgoverning the creation and growth as well as processes taking place onnetworks, like e.g. the Internet, transportation or neural networks. It turnedout that most real-world networks cannot be simply reduced to a compound ofsome individual components. Fortunately, the statistical mechanics, being oneof pillars of modern physics, provides us with a very powerful set of tools andmethods for describing and understanding these systems. In this thesis, wewould like to present a consistent approach to complex networks based onstatistical mechanics, with the central role played by the concept ofstatistical ensemble of networks. We show how to construct such a theory andpresent some practical problems where it can be applied. Among them, we payattention to the problem of finite-size corrections and the dynamics of asimple model of mass transport on networks.


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Input: We investigate the dimerization and fusion of C60 molecules to form variousC60 dimers when pushed against each other at several inter-molecular distances.We study the stability of this dimerized C60 molecule based on its bindingstrength provided by intramolecular interactions. Tersoff potential, which isconsidered to represent intramolecular interactions well, has been used tocalculate potential energy at these distances of separation and for allpossible orientations of the molecules. We observe that several minimum energyconfigurations exist at various distances between the C60 molecules. Ourcalculation shows that apart from the dumbbell structures, many interestingcomposite phases also result, such as fused, peanut and carbon nanotubes ofgeometry (5,5) and (10,0) of certain specific length.


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Input: Recently in \cite{jss1}, the authors have given a method for calculation ofthe effective resistance (resistance distance) on distance-regular networks,where the calculation was based on stratification introduced in \cite{js} andStieltjes transform of the spectral distribution (Stieltjes function)associated with the network. Also, in Ref. \cite{jss1} it has been shown thatthe resistance distances between a node $\alpha$ and all nodes $\beta$belonging to the same stratum with respect to the $\alpha$($R_{\alpha\beta^{(i)}}$, $\beta$ belonging to the $i$-th stratum with respectto the $\alpha$) are the same. In this work, an algorithm for recursivecalculation of the resistance distances in an arbitrary distance-regularresistor network is provided, where the derivation of the algorithm is based onthe Bose-Mesner algebra, stratification of the network, spectral techniques andChristoffel-Darboux identity. It is shown that the effective resistance on adistance-regular network is an strictly increasing function of the shortestpath distance defined on the network. In the other words, the two-pointresistance $R_{\alpha\beta^{(m+1)}}$ is strictly larger than$R_{\alpha\beta^{(m)}}$. The link between the resistance distance and randomwalks on distance-regular networks is discussed, where the average commute time(CT) and its square root (called Euclidean commute time (ECT)) as a distanceare related to the effective resistance. Finally, for some important examplesof finite distance- regular networks, the resistance distances are calculated.  {\bf Keywords: resistance distance, association scheme, stratification,distance-regular networks, Christoffel-Darboux identity}  {\bf PACs Index: 01.55.+b, 02.10.Yn}


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Input: This paper uncovers and explores the close relationship between Monte CarloOptimization of a parametrized integral (MCO), Parametric machine-Learning(PL), and `blackbox' or `oracle'-based optimization (BO). We make fourcontributions. First, we prove that MCO is mathematically identical to a broadclass of PL problems. This identity potentially provides a new applicationdomain for all broadly applicable PL techniques: MCO. Second, we introduceimmediate sampling, a new version of the Probability Collectives (PC) algorithmfor blackbox optimization. Immediate sampling transforms the original BOproblem into an MCO problem. Accordingly, by combining these first twocontributions, we can apply all PL techniques to BO. In our third contributionwe validate this way of improving BO by demonstrating that cross-validation andbagging improve immediate sampling. Finally, conventional MC and MCO proceduresignore the relationship between the sample point locations and the associatedvalues of the integrand; only the values of the integrand at those locationsare considered. We demonstrate that one can exploit the sample locationinformation using PL techniques, for example by forming a fit of the samplelocations to the associated values of the integrand. This provides anadditional way to apply PL techniques to improve MCO.


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Input: High resolution molecular line observations of CS, HCO+, C18O and N2H+ wereobtained toward the starless globule FeSt 1-457 in order to investigate itskinematics and chemistry. The HCO+ and CS spectra show clear self-reversed andasymmetric profiles across the face of the globule. The sense of the observedasymmetry is indicative of the global presence of expansion motions in theouter layers of the globule. These motions appear to be subsonic andsignificantly below the escape velocity of the globule. Comparison of ourobservations with near-infrared extinction data indicate that the globule isgravitationally bound. Taken together these considerations lead us to suggestthat the observed expansion has its origin in an oscillatory motion of theouter layers of the globule which itself is likely in a quasi-stable state nearhydrostatic equilibrium. Analysis of the observed linewidths of CO and N2H+confirm that thermal pressure is the dominant component of the cloud's internalsupport. A simple calculation suggests that the dominant mode of pulsationwould be an l = 2 mode with a period of 0.3 Myr. Deformation of the globule dueto the large amplitude l = 2 oscillation may be responsible for thedouble-peaked structure of the core detected in high resolution extinctionmaps. Detailed comparison of the molecular-line observations and extinctiondata provides evidence for significant depletion of C18O and perhaps HCO+ whileN2H+ may be undepleted to a cloud depth of about 40 magnitudes of visualextinction.


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Input: We discuss the results from the combined IRAC and MIPS c2d Spitzer Legacyobservations of the Serpens star-forming region. In particular we present a setof criteria for isolating bona fide young stellar objects, YSO's, from theextensive background contamination by extra-galactic objects. We then discussthe properties of the resulting high confidence set of YSO's. We find 235 suchobjects in the 0.85 deg^2 field that was covered with both IRAC and MIPS. Anadditional set of 51 lower confidence YSO's outside this area is identifiedfrom the MIPS data combined with 2MASS photometry. We describe two sets ofresults, color-color diagrams to compare our observed source properties withthose of theoretical models for star/disk/envelope systems and our own modelingof the subset of our objects that appear to be star+disks. These objectsexhibit a very wide range of disk properties, from many that can be fit withactively accreting disks to some with both passive disks and even possiblydebris disks. We find that the luminosity function of YSO's in Serpens extendsdown to at least a few x .001 Lsun or lower for an assumed distance of 260 pc.The lower limit may be set by our inability to distinguish YSO's fromextra-galactic sources more than by the lack of YSO's at very low luminosities.A spatial clustering analysis shows that the nominally less-evolved YSO's aremore highly clustered than the later stages and that the backgroundextra-galactic population can be fit by the same two-point correlation functionas seen in other extra-galactic studies. We also present a table of matchesbetween several previous infrared and X-ray studies of the Serpens YSOpopulation and our Spitzer data set.


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Input: We investigate the problem of vortex trapping in cyclically coupledBose-Josephson junctions. Starting with $N$ independent BECs we couple thecondensates through Josephson links and allow the system to reach a stablecirculation by adding a dissipative term in our semiclassical equations ofmotion. The central question we address is what is the probability to trap avortex with winding number $m$. Our numerical simulations reveal that the finaldistribution of winding numbers is narrower than the initial distribution oftotal phases, indicating an increased probability for no-vortex configurations.Further, the nonlinearity of the problem manifests itself in the somewhatcounter-intuitive result that it is possible to obtain a non-zero circulationstarting with zero total phase around the loop. The final width of thedistribution of winding numbers for $N$ sites scales as $\lambda N^{\alpha}$,where $\alpha=0.47\pm 0.01$ and $\lambda <0.67$ (value predicted for theinitial distribution) indicating a shrinking of the final distribution. Theactual value of $\lambda$ is found to depend on the strength of dissipation.


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Input: In the present paper a plastic-damage model for concrete is discussed. Basedon the fact that for isotropic materials the elastic trial stress and theprojected plastic stress states have the same eigenvec-tors, the loadingsurface is formulated in the principal stress space rather than using theinvariants of stress tensor. The model assumes that the directions oforthotropic damage coincide with principal directions of elastic predictorstress state (motivated by coaxial rotated crack model). Due to thisassumption, the load-ing surface and the closest point projection algorithm canstill be formulated in the principal directions. The evolution of the inelasticstrain is determined using minimization principle. Damage and plastic parts ofthe inelastic strain are separated using a scalar parameter, which is assumedto be stress dependent. The paper also discusses an effective numericalimplementation. The performance of the model is demonstrated on oneillustrative example.


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Input: We have measured resonance strengths and energies for dielectronicrecombination (DR) of Mg-like Fe XV forming Al-like Fe XIV via N=3 -> N' = 3core excitations in the electron-ion collision energy range 0-45 eV. Allmeasurements were carried out using the heavy-ion Test Storage Ring at the MaxPlanck Institute for Nuclear Physics in Heidelberg, Germany. We have alsocarried out new multiconfiguration Breit-Pauli (MCBP) calculations using theAUTOSTRUCTURE code. For electron-ion collision energies < 25 eV we find pooragreement between our experimental and theoretical resonance energies andstrengths. From 25 to 42 eV we find good agreement between the two forresonance energies. But in this energy range the theoretical resonancestrengths are ~ 31% larger than the experimental results. This is larger thanour estimated total experimental uncertainty in this energy range of +/- 26%(at a 90% confidence level). Above 42 eV the difference in the shape betweenthe calculated and measured 3s3p(^1P_1)nl DR series limit we attribute partlyto the nl dependence of the detection probabilities of high Rydberg states inthe experiment. We have used our measurements, supplemented by ourAUTOSTRUCTURE calculations, to produce a Maxwellian-averaged 3 -> 3 DR ratecoefficient for Fe XV forming Fe XIV. The resulting rate coefficient isestimated to be accurate to better than +/- 29% (at a 90% confidence level) fork_BT_e > 1 eV. At temperatures of k_BT_e ~ 2.5-15 eV, where Fe XV is predictedto form in photoionized plasmas, significant discrepancies are found betweenour experimentally-derived rate coefficient and previously publishedtheoretical results. Our new MCBP plasma rate coefficient is 19-28% smallerthan our experimental results over this temperature range.