A5085823033- Quantum Chromodynamics and Particle Interactions
- Pulsars and Gravitational Waves Research
- Nuclear physics research studies
- High-Energy Particle Collisions Research
- Particle physics theoretical and experimental studies
- Gamma-ray bursts and supernovae
- High-pressure geophysics and materials
- Cold Atom Physics and Bose-Einstein Condensates
- Geophysics and Gravity Measurements
- Dark Matter and Cosmic Phenomena
- Quantum, superfluid, helium dynamics
- Atomic and Subatomic Physics Research
- Superconducting Materials and Applications
- Neutrino Physics Research
- Astro and Planetary Science
- Physics of Superconductivity and Magnetism
- Quantum and electron transport phenomena
- earthquake and tectonic studies
- Astrophysics and Cosmic Phenomena
- Atomic and Molecular Physics
- Polynomial and algebraic computation
- Quantum chaos and dynamical systems
- Advanced NMR Techniques and Applications
- Inertial Sensor and Navigation
- Stellar, planetary, and galactic studies
Nankai University
2016-2025
Tianjin University
2019-2022
University of Illinois Urbana-Champaign
2020-2021
Osaka University
1997-2020
Institute of High Energy Physics
1995-2020
China Electric Power Research Institute
2013
North China Electric Power University
2013
University of Washington
2009-2011
Yangzhou Polytechnic Institute
2005-2009
The University of Adelaide
2007
We construct the equation of state (EOS) nuclear matter at finite temperature and density with various proton fractions within relativistic mean field (RMF) theory for use in supernova simulations. The Thomas-Fermi approximation is adopted to describe non-uniform where we consider nucleus, alpha-particle, neutron equilibrium. treat uniform consistently using RMF theory. tabulate outcome as pressure, free energy, entropy etc, enough mesh points wide ranges temperature, fraction, baryon mass density.
We study the evolution of supernova core from beginning gravitational collapse a 15Msolar star up to 1 second after bounce. present results spherically symmetric simulations core-collapse supernovae by solving general relativistic neutrino-radiation-hydrodynamics in implicit time-differencing. aim explore shock wave long term and investigate formation protoneutron together with neutrino signatures. These studies are done examine influence equation state (EOS) on postbounce late phase...
We construct the equation of state (EOS) dense matter covering a wide range temperature, proton fraction, and density for use core-collapse supernova simulations. The study is based on relativistic mean-field (RMF) theory, which can provide an excellent description nuclear finite nuclei. Thomas–Fermi approximation in combination with assumed nucleon distribution functions free energy minimization adopted to describe non-uniform matter, composed lattice heavy treat uniform consistently using...
Abstract We construct a new equation of state (EOS) for numerical simulations core-collapse supernovae and neutron-star mergers based on an extended relativistic mean-field model with small symmetry energy slope L , which is compatible both experimental nuclear data recent observations neutron stars. The EOS table (EOS4) the TM1 (TM1e) = 40 MeV designed in same tabular form compared commonly used Shen (EOS2) original . This convenient useful performing examining influences its density...
Abstract We investigate the influence of effective nucleon mass on equation state (EOS), which is constructed for simulations core-collapse supernovae and binary neutron star mergers, within relativistic mean-field (RMF) framework. The study introduces a new RMF parameter set, TM1m, modification TM1e model with an adjusted mass, maintaining saturation properties nuclear matter. TM1m model, larger ratio ( M * / ~ 0.8) compared to 0.63), employed construct EOS table, EOS5. This table designed...
Using the upgraded Beijing Spectrometer, we have measured total cross section for e+e− annihilation into hadronic final states at center-of-mass energies of 2.6, 3.2, 3.4, 3.55, 4.6, and 5.0 GeV. Values R, σ(e+e−→hadrons)/σ(e+e−→μ+μ−), are determined.Received 28 July 1999DOI:https://doi.org/10.1103/PhysRevLett.84.594©2000 American Physical Society
The BES experiment at the Beijing electron-positron collider has observed ξ(2230) signal in π+π−, K+K−, K0SK0S, and p¯p final states with 4.6σ, 4.1σ, 4.0σ, 3.8σ statistical significances, respectively. new observations of two nonstrange decay modes ξ→π+π− are important evidence for glueball interpretation ξ(2230).Received 30 October 1995DOI:https://doi.org/10.1103/PhysRevLett.76.3502©1996 American Physical Society
We study the hadron-quark phase transition in interior of neutron stars. The relativistic mean field (RMF) theory is adopted to describe hadronic matter phase, while Nambu-Jona-Lasinio (NJL) model used for quark phase. influence equation state on and star properties are investigated. find that a possesses large population hyperons, but it not dense enough possess pure core. Whether mixed exist core stars depends RMF parameters used.
We study the effects of symmetry energy on neutron drip density and properties nuclei in star crusts. The nonuniform matter around point is calculated by using Thomas--Fermi approximation with relativistic mean-field model. composition crust are found to be correlated its slope. compare self-consistent other treatments surface Coulomb energies find that these finite-size play an essential role determining equilibrium state at low density.
We construct the equation of state (EOS) in a wide density range for neutron stars using relativistic mean field theory. The properties star matter with both uniform and non-uniform distributions are studied consistently. inclusion hyperons considerably softens EOS at high densities. Thomas-Fermi approximation is used to describe matter, which composed lattice heavy nuclei. phase transition from occurs around $0.06 \rm{fm^{-3}}$, free neutrons drip out nuclei about $2.4 \times 10^{-4}\...
We investigate the effects of symmetry energy on nuclear pasta phases and crust-core transition in neutron stars. employ relativistic mean-field approach coexisting method to study properties presented inner crust It is found that slope at saturation density plays an important role phase properties. The correlation between obtained this consistent with those by other methods.
We study the finite-size effects, like surface and Coulomb energies, on hadron-quark mixed phase in neutron stars. The equilibrium conditions for coexisting hadronic quark phases are derived by minimizing total energy including contributions, which different from Gibbs without effects. employ relativistic mean-field model to describe phase, while Nambu-Jona-Lasinio with vector interactions is used phase. It found that effects can significantly reduce region of results lie between those...
We study the hadron-quark mixed phase, which may occur in interior of neutron stars. The relativistic mean-field model is employed to describe hadronic while Nambu-Jona-Lasinio used for quark phase. examine effects nuclear symmetry energy phase and repulsive vector interaction For treatment we compare four methods: (1) minimization method, (2) coexisting phases (3) Gibbs construction, (4) Maxwell construction. finite-size like surface Coulomb energies are taken into account methods, play a...
We explore the possibility of a structured hadron-quark mixed phase forming in interior neutron stars. The quark-meson coupling (QMC) model, which explicitly incorporates internal quark structure nucleon, is employed to describe hadronic phase, while described by same bag model as one used QMC framework, so keep consistency between two coexisting phases. analyze effect appearance pasta phases on neutron-star properties. also discuss influence nuclear symmetry energy and constant $B$ matter...
It is of great interest to understand the equation state (EOS) neutron star (NS), whose core includes highly dense matter. However, there are large uncertainties in theoretical predictions for EOS NS. useful develop a new framework, which flexible enough consider systematic error and use them as best guess at same time. We employ deep neural network perform non-parametric fit NS using currently available data. In this Gaussian process applied represent EOSs training set data required close...
A recent report has identified a central compact object (CCO) within the supernova remnant HESS J1731-347, with mass and radius of $M={0.77}_{\ensuremath{-}0.17}^{+0.20}{M}_{\ensuremath{\bigodot}}$ $R={10.4}_{\ensuremath{-}0.78}^{+0.86}\text{ }\text{ }\mathrm{km}$, respectively. To investigate this light star, density-dependent relativistic mean-field (DDRMF) model, specifically DDVT been employed. The model incorporates tensor couplings vector mesons, which can successfully describe...
We study the properties of double-Λ hypernuclei in relativistic mean-field theory, which has been successfully used for description stable and unstable nuclei. With meson-hyperon couplings determined by experimental binding energies single-Λ hypernuclei, we present a self-consistent calculation discuss influence hyperons on nuclear core. The contribution two mesons with dominant strange quark components (scalar σ* vector φ) to ΛΛ energy is examined.
We study the $^1S_0$ superfluidity of $\Lambda$ hyperons in neutron star matter and stars. use relativistic mean field (RMF) theory to calculate properties matter. In RMF approach, meson-hyperon couplings are constrained by reasonable hyperon potentials that include updated information from recent developments hypernuclear physics. To examine pairing gap hyperons, we employ several $\Lambda\Lambda$ interactions based on Nijmegen models used double-$\Lambda$ hypernuclei studies. It is found...
We study the impact of symmetry energy on properties nuclear pasta phases and crust-core transition in neutron stars. perform a self-consistent Thomas-Fermi calculation employing relativistic mean-field model. The presented inner crust stars are investigated is examined. It found that slope plays an important role determining phase structure transition. correlation between density obtained approximation consistent with predicted by liquid-drop
We study the effects of nuclear symmetry energy on mass-radius relation and tidal deformability neutron stars, considering self-consistency equation state (EOS). first construct a set unified EOSs based relativistic mean-field models with different density dependence energy. For description pasta phases appearing in inner crust we perform self-consistent Thomas-Fermi calculation using same interaction as that for uniform matter core. To examine possible from EOS neutron-star properties,...
We investigate systematically the quark-hadron mixed phase in dense stellar matter and its influence on compact star structures. The properties of quark hadronic are fixed based various model predictions. Beside adopting constant values, surface tension $\mathrm{\ensuremath{\Sigma}}$ for interface is estimated with multiple reflection expansion method equivparticle model. To fix structures pasta phases, a continuous dimensionality structure adopted as proposed by Ravenhall et al....