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Yue Shen

Publications and source records attributed to Yue Shen.

At least 325 records · Page 18Linked to original sources
arXiv2007

Do broad absorption line quasars live in different environments from ordinary quasars?

We select a sample of $\sim 4200$ traditionally defined broad absorption line quasars (BALQs) from the Fifth Data Release quasar catalog of the Sloan Digital Sky Survey. For a statistically homogeneous quasar sample with $1.7\le z\le 4.2$, the BAL quasar fraction is $\sim 14%$ and is almost constant with redshift. We measure the auto-correlation of non-BAL quasars (nonBALQs) and the cross-correlation of BALQs with nonBALQs using this statistically homogeneous sample, both in redshift space and using the projected correlation function. We find no significant difference between the clustering strengths of BALQs and nonBALQs. Assuming a power-law model for the real space correlation function $ξ(r)=(r/r_0)^{-1.8}$, the correlation length for nonBALQs is $r_0=7.6\pm 0.8 h^{-1}{\rm Mpc}$; for BALQs, the cross-correlation length is $r_0=7.4\pm 1.1 h^{-1}{\rm Mpc}$. Our clustering results suggest that BALQs live in similar large-scale environments as do nonBALQs.

astro-ph↗
arXiv2007

The Sloan Digital Sky Survey Quasar Catalog IV. Fifth Data Release

We present the fourth edition of the Sloan Digital Sky Survey (SDSS) Quasar Catalog. The catalog contains 77,429 objects; this is an increase of over 30,000 entries since the previous edition. The catalog consists of the objects in 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 have interesting/complex absorption features, are fainter than i=15.0, and have highly reliable redshifts. The area covered by the catalog is 5740 sq. deg. The quasar redshifts range from 0.08 to 5.41, with a median value of 1.48; the catalog includes 891 quasars at redshifts greater than four, of which 36 are at redshifts greater than five. Approximately half of the catalog quasars have i < 19; nearly all have i < 21. For each object the catalog presents positions accurate 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 the morphology 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 the wavelength region 3800--9200A at a spectral resolution of ~2000. The spectra can be retrieved from the public database using the information provided in the catalog. The average SDSS colors of quasars as a function of redshift, derived from the catalog entries, are presented in tabular form. Approximately 96% of the objects in the catalog were discovered by the SDSS.

astro-ph↗
arXiv2007

Clustering of High Redshift ($z\ge 2.9$) Quasars from the Sloan Digital Sky Survey

(Abridged) We study the two-point correlation function of a uniformly selected sample of 4,426 luminous optical quasars with redshift $2.9 \le z\le 5.4$ selected over 4041 deg$^2$ from the Fifth Data Release of the Sloan Digital Sky Survey. For a real-space correlation function of the form $ξ(r)=(r/r_0)^{-γ}$, the fitted parameters in comoving coordinates are $r_0 = 15.2 \pm 2.7 h^{-1}$ Mpc and $γ= 2.0 \pm 0.3$, over a scale range $4\le r_p\le 150 h^{-1}$ Mpc. Thus high-redshift quasars are appreciably more strongly clustered than their $z \approx 1.5$ counterparts, which have a comoving clustering length $r_0 \approx 6.5 h^{-1}$ Mpc. Dividing our sample into two redshift bins: $2.9\le z\le 3.5$ and $z\ge 3.5$, and assuming a power-law index $γ=2.0$, we find a correlation length of $r_0 = 16.9 \pm 1.7 h^{-1}$ Mpc for the former, and $r_0 = 24.3 \pm 2.4 h^{-1}$ Mpc for the latter. Following Martini & Weinberg, we relate the clustering strength and quasar number density to the quasar lifetimes and duty cycle. Using the Sheth & Tormen halo mass function, the quasar lifetime is estimated to lie in the range $4\sim 50$ Myr for quasars with $2.9\le z\le 3.5$; and $30\sim 600$ Myr for quasars with $z\ge 3.5$. The corresponding duty cycles are $0.004\sim 0.05$ for the lower redshift bin and $0.03\sim 0.6$ for the higher redshift bin. The minimum mass of halos in which these quasars reside is $2-3\times 10^{12}\ h^{-1}M_\odot$ for quasars with $2.9\le z\le 3.5$ and $4-6\times 10^{12}\ h^{-1}M_\odot$ for quasars with $z\ge 3.5$.

astro-ph↗
arXiv2006

Differences in the AGN Populations of Groups and Clusters: Clues to AGN Evolution

We combine optical and X-ray data for eight low redshift ($z\sim 0.06$) poor groups of galaxies from the {\it XI}({\it XMM/IMACS}) Groups Project to study the AGN population in the group environment. Among $\sim 140$ group members, we identify five AGN based on their optical emission lines. None of these optically-selected AGN are detected by {\it XMM-Newton}. One additional AGN is discovered in the {\it XMM-Newton} observations. This X-ray detected AGN, which has no obvious AGN emission line signatures in its optical spectrum, is a member of the only X-ray luminous group in our sample. The lack of a significant population of X-ray bright, but optically dull AGN among less dynamically evolved groups is in stark contrast to the large fraction of such objects in rich clusters of galaxies (Martini et al. 2006). We suggest this result can be explained by a physical scenario for AGN accretion evolution: AGN activity is initially triggered by galaxy merging, leading to a high accretion rate and an optically dominant phase (via thin disk accretion). As the accretion rate drops in time, the AGN gradually enters an X-ray dominant low-accretion phase (via a radiative inefficient accretion flow). In this picture, optical- and X-ray-selected AGN are the same population of supermassive black holes observed at different epochs. Within the context of this scenario, the majority of AGN in poor groups are in the high-accretion optically dominant phase, while the AGN population in rich clusters is mostly in the low-accretion X-ray dominant phase.

astro-ph↗
arXiv2006

Three Dimensional Compressible Hydrodynamic Simulations of Vortices in Disks

We carry out three-dimensional, high resolution (up to $1024^2\times 256$) hydrodynamic simulations of the evolution of vortices in vertically unstratified Keplerian disks using the shearing sheet approximation. The transient amplification of incompressible, linear amplitude leading waves (which has been proposed as a possible route to nonlinear hydrodynamical turbulence in disks) is used as one test of our algorithms; our methods accurately capture the predicted amplification, converges at second-order, and is free from aliasing. Waves expected to reach nonlinear amplitude at peak amplification become unstable to Kelvin-Helmholtz modes when $\mid W_{\rm max}\mid\gtrsim Ω$ (where $W_{\rm max}$ is the local maximum of vorticity and $Ω$ the angular velocity). We study the evolution of a power-law distribution of vorticity consistent with Kolmogorov turbulence; in two-dimensions long-lived vortices emerge and decay slowly, similar to previous studies. In three-dimensions, however, vortices are unstable to bending modes, leading to rapid decay. Only vortices with a length to width ratio smaller than one survive; in three-dimensions the residual kinetic energy and shear stress is at least one order of magnitude smaller than in two-dimensions. No evidence for sustained hydrodynamical turbulence and transport is observed in three-dimensions. Instead, at late times the residual transport is determined by the amplitude of slowly decaying, large-scale vortices (with horizontal extent comparable to the scale height of the disk), with additional contributions from nearly incompressible inertial waves possible. Evaluating the role that large-scale vortices play in astrophysical accretion disks will require understanding the mechanisms that generate and destroy them.

astro-ph↗
arXiv2006

Dispersal of Gaseous Circumstellar Discs around High-Mass Stars

We study the dispersal of a gaseous disc surrounding a central high-mass stellar core once this circumstellar disc becomes fully ionized. If the stellar and surrounding EUV and X-ray radiations are so strong as to rapidly heat up and ionize the entire circumstellar disc as further facilitated by disc magnetohydrodynamic (MHD) turbulence, a shock can be driven to travel outward in the fully ionized disc, behind which the disc expands and thins. For an extremely massive and powerful stellar core, the ionized gas pressure overwhelms the centrifugal and gravitational forces in the disc. In this limit, we construct self-similar shock solutions for such an expansion and depletion phase. As a significant amount of circumstellar gas being removed, the relic disc becomes vulnerable to strong stellar winds and fragments into clumps. We speculate that disc disappearance happens rapidly, perhaps on a timescale of $\sim 10^3-10^4\hbox{yr}$ once the disc becomes entirely ionized sometime after the onset of thermal nuclear burning in a high-mass stellar core.

astro-ph↗
arXiv2005

Forming supermassive black holes by accreting dark and baryon matter

Given a large-scale mixture of self-interacting dark matter (SIDM) particles and baryon matter distributed in the early Universe, we advance here a two-phase accretion scenario for forming supermassive black holes (SMBHs) with masses around $\sim 10^9 M_{\odot}$ at high redshifts $z (\gsim 6)$. The first phase is conceived to involve a rapid quasi-spherical and quasi-steady Bondi accretion of mainly SIDM particles embedded with baryon matter onto seed black holes (BHs) created at redshifts $z\lsim 30$ by the first generation of massive Population III stars; this earlier phase rapidly gives birth to significantly enlarged seed BH masses of $M_{\hbox{\tiny BH},t_1}\backsimeq 1.4\times 10^6\ M_\odot σ_0/(1\hbox{cm}^2\hbox{g}^{-1})(C_s/30\hbox{km s}^{-1})^4$ during $z\sim 20-15$, where $σ_0$ is the cross section per unit mass of SIDM particles and $C_s$ is the velocity dispersion in the SIDM halo referred to as an effective "sound speed". The second phase of BH mass growth is envisaged to proceed primarily via baryon accretion, eventually leading to SMBH masses of $M_{\hbox{\tiny BH}}\sim 10^9 M_\odot$; such SMBHs may form either by $z\sim 6$ for a sustained accretion at the Eddington limit or later at lower $z$ for sub-Eddington mean accretion rates. We intend to account for the reported detections of a few SMBHs at early epochs, e.g., SDSS 1148+5251 and so forth, without necessarily resorting to either super-Eddington baryon accretion or very frequent BH merging processes. Only extremely massive dark SIDM halos associated with rare peaks of density fluctuations in the early Universe may harbour such early SMBHs or quasars. Observational consequences are discussed.

astro-ph↗
arXiv2004

Structures in a class of magnetized scale-free discs

We construct analytically stationary global configurations for both aligned and logarithmic spiral coplanar magnetohydrodynamic (MHD) perturbations in an axisymmetric background MHD disc with a power-law surface mass density $Σ_0\propto r^{-α}$, a coplanar azimuthal magnetic field $B_0\propto r^{-γ}$, a consistent self-gravity and a power-law rotation curve $v_0\propto r^{-β}$ where $v_0$ is the linear azimuthal gas rotation speed. The barotropic equation of state $Π\proptoΣ^{n}$ is adopted for both MHD background equilibrium and coplanar MHD perturbations where $Π$ is the vertically integrated pressure and $n$ is the barotropic index. For a scale-free background MHD equilibrium, a relation exists among $α$, $β$, $γ$ and $n$ such that only one parameter (e.g., $β$) is independent. For a linear axisymmetric stability analysis, we provide global criteria in various parameter regimes. For nonaxisymmetric aligned and logarithmic spiral cases, two branches of perturbation modes (i.e., fast and slow MHD density waves) can be derived once $β$ is specified. To complement the magnetized singular isothermal disc (MSID) analysis of Lou, we extend the analysis to a wider range of $-1/4<β<1/2$. As an example of illustration, we discuss specifically the $β=1/4$ case when the background magnetic field is force-free. Angular momentum conservation for coplanar MHD perturbations and other relevant aspects of our approach are discussed.

astro-ph↗
arXiv2004

Outflows and inflows in astrophysical systems

We seek for self-similar solutions describing the time-dependent evolution of self-gravity systems with either spherical symmetry or axisymmetric disk geometry. By assuming self-similar variable $x\equiv r/at$ where $a$ is isothermal sound speed we find self-similar solutions extending from the initial instant $t=0$ to the final stage $t\to \infty$ using standard semi-analytical methods. Different types of solutions are constructed, which describe overall expansion or collapse, envelope expansion with core collapse (EECC), the formation of central rotationally supported quasi-equilibrium disk as well as shocks. Though infinitely many, these self-similarity solutions have similar asymptotic behaviors which may impose diagnosis on the velocity and density structures in astrophysical systems.

astro-ph↗
arXiv2004

Shocked similarity collapses and flows in star formation processes

We propose self-similar shocked flow models for certain dynamical evolution phases of young stellar objects (YSOs), `champagne flows' of H {\sevenrm II} regions surrounding OB stars and shaping processes of planetary nebulae (PNe). We analyze an isothermal fluid of spherical symmetry and construct families of similarity shocked flow solutions featured by: 1. either a core expansion with a finite central density or a core accretion at constant rate with a density scaling $\propto r^{-3/2}$; 2. a shock moving outward at a constant speed; 3. a preshock gas approaching a constant speed at large $r$ with a density scaling $\propto r^{-2}$. In addition to testing numerical codes, our models can accommodate diverse shocked flows with or without a core collapse or outflow and an envelope expansion or contraction. As an application, we introduce our model analysis to observations of Bok globule B335.

astro-ph↗
arXiv2004

Global axisymmetric stability analysis for a composite system of two gravitationally coupled scale-free discs

In a composite system of gravitationally coupled stellar and gaseous discs, we perform linear stability analysis for axisymmetric coplanar perturbations using the two-fluid formalism. The background stellar and gaseous discs are taken to be scale-free with all physical variables varying as powers of cylindrical radius $r$ with compatible exponents. The unstable modes set in as neutral modes or stationary perturbation configurations with angular frequency $ω=0$.

astro-ph↗
arXiv2004

Gravitationally coupled scale-free discs

In a composite fluid system of two gravitationally coupled barotropic scale-free discs bearing a rotation curve $v\propto r^{-β}$ and a power-law surface mass density $Σ_0\propto r^{-α}$ with $α=1+2β$, we construct coplanar stationary aligned and spiral perturbation configurations in the two discs. Due to the mutual gravitational interaction, there are two independent classes of perturbation modes with surface mass density disturbances in the two coupled discs being either in-phase or out-of-phase. We derive analytical criteria for such perturbation modes to exist and show numerical examples. We compute the aligned and spiral perturbation modes systematically to explore the entire parameter regime. For the axisymmetric $m=0$ case with radial oscillations, there are two unstable regimes of ring-fragmentation and collapse corresponding to short and long radial wavelengths, respectively. Only within a certain range of the rotation parameter $D_s^2$ (square of the effective Mach number for the stellar disc), can a composite disc system be stable against all axisymmetric perturbations. Compared with a single-disc system, the coupled two-disc system becomes less stable against such axisymmetric instabilities.

astro-ph↗
arXiv2003

Envelope Expansion with Core Collapse. I. Spherical Isothermal Similarity Solutions

We investigate self-similar dynamical processes in an isothermal self-gravitational fluid with spherical symmetry. In reference to earlier complementary solution results of Larson, Penston, Shu, Hunter and Whitworth & Summers, we further explore the `semi-complete solution space' from an initial instant $t\to 0^{+}$ to a final stage $t\to +\infty$. These similarity solutions can describe and accommodate physical processes of radial inflow, core collapse, oscillations and envelope expansion (namely, outflow or wind) or contraction as well as shocks. In particular, we present new classes of self-similar solutions, referred to as `envelope expansion with core collapse' (EECC) solutions, that are featured by an interior core collapse and an exterior envelope expansion concurrently. The interior collapse towards the central core approaches a free-fall state as the radius $r\to 0$, while the exterior envelope expansion gradually approaches a constant radial flow speed as $r\to +\infty$. There exists at least one spherical stagnation surface of zero flow speed that separates the core collapse and the envelope outflow and that travels outward at constant speed, either subsonically or supersonically, in a self-similar manner.

astro-ph↗
arXiv2003

Theoretical study on RbCl crystal with Möbius inverse potentials

The alkali halides have been studied very frequently for their simple structures and interesting properties, for example, the high-pressure induced transition$^1$. There are several successful models that can be employed. The most famous model of them is the Tosi-Fumi interionic potential$^2$ which is an empirical potential derived from the experimental data. Whereas, here we developed a new potential model based on the Möbius lattice inversion method$^{3,4}$, which can be derived directly from the cohesive energy curve without any experimental data and is more effective than the ab initial calculation. With the Möbius interionic potentials, we calculated the structural and elastic properties of RbCl crystal. The results are in good agreement with experiments. We also studied the high-pressure induced B1-B2 transition of RbCl crystal and estimated approximately the transition-point which is about 1.09GPa. Further more, we used this potential model to simulate the RbCl melting with molecular dynamics. The calculated melt-point is approximately 990K$\sim$995K, close to the experimental data.

cond-mat.mtrl-sci↗
arXiv2003

Perturbation configurations in a two-fluid system of singular isothermal disks

We investigate properties of stationary aligned and unaligned spiral perturbation configurations in a composite system of gravitationally coupled stellar and gaseous singular isothermal disks (SIDs) using the two-fluid formalism. We obtain stationary perturbation solutions for aligned and unaligned spiral logarithmic configurations in such a composite SID system and derive analytically existence criteria for these solutions. In comparison with the similar problem of a single SID studied by Shu et al. (2000), there are now two possible sets of solutions owing to an additional SID.

astro-ph↗
arXiv1994

Chirally Extended Quantum Chromodynamics

We propose an extended Quantum Chromodynamics (XQCD) Lagrangian in which the fermions are coupled to elementary scalar %$σ$ and $π$ fields through a Yukawa coupling which preserves chiral invariance. Our principle motivation is to find a new lattice formulation for QCD which avoids the source of critical slowing down usually encountered as the bare quark mass is tuned to the chiral limit. The phase diagram and the weak coupling limit for XQCD are studied. They suggest a conjecture that the continuum limit of XQCD is the same as the continuum limit of conventional lattice formulation of QCD. As examples of such universality, we present the large N solutions of two prototype models for XQCD, in which the mass of the spurious pion and sigma resonance go to infinity with the cut-off. Even if the universality conjecture turns out to be false, we believe that XQCD will still be useful as a low energy effective action for QCD phenomenology on the lattice. Numerical simulations are recommended to further investigate the possible benefits of XQCD in extracting QCD predictions. Postscript files for figures are attached. Search for strings "fig11.ps", "fig22.ps", "fig33.ps".

hep-lat↗
arXiv1993

Isgur-Wise Function on the Lattice

We review our method and numerical results for calculation of the Isgur-Wise function on the lattice. We present a discussion of the systematic errors. Using recent experimental results, we find $V_{cb} = 0.044\pm 0.005\pm .007$. Contribution to Lattice '93 proceedings. Needs espcrc2.sty file (included after \end{document}). Search Figure1.ps for postscript files.

hep-lat↗