Astrophysical constraints on a parametric equation of state for neutron-rich nucleonic matter  

作　　者：Nai-Bo Zhang Bao-An Li 

机构地区：[1]Shandong Provincial Key Laboratory of Optical Astronomy and Solar-Terrestrial Environment, School of Space Science and Physics, Institute of Space Sciences, Shandong University [2]Department of Physics and Astronomy, Texas A&M University-Commerce

出　　处：《Nuclear Science and Techniques》2018年第12期62-70,共9页核技术（英文）

基　　金：NBZ was supported in part by the China Scholarship Council;the U.S.Department of Energy,Office of Science,under Award Number DE-SC0013702,the CUSTIPEN(China-U.S.Theory Institute for Physics with Exotic Nuclei)under the U.S.Department of Energy Grant No.DE-SC0009971;the National Natural Science Foundation of China under Grant No.11320101004

摘　　要：Extracting the equation of state(EOS) and symmetry energy of dense neutron-rich matter from astrophysical observations is a long-standing goal of nuclear astrophysics. To facilitate the realization of this goal, the feasibility of using an explicitly isospin-dependent parametric EOS for neutron star matter was investigated recently in [1–3]. In this contribution, in addition to outlining the model framework and summarizing the most important findings from [1–3], we report a few new results regarding constraining parameters characterizing the highdensity behavior of nuclear symmetry energy. In particular,the constraints on the pressure of neutron star matter extracted from combining the X-ray observations of the neutron star radius, the minimum–maximum mass M=2:01 M_⊙, and causality condition agree very well with those extracted from analyzing the tidal deformability data by the LIGO ? Virgo Collaborations. The limitations of using the radius and/or tidal deformability of neutron stars to constrain the high-density nuclear symmetry energy are discussed.Extracting the equation of state （EOS） and symmetry energy of dense neutron-rich matter from astrophysical observations is a long-standing goal of nuclear astrophysics. To facilitate the realization of this goal, the feasibility of using an explicitly isospin-depen- dent parametric EOS for neutron star matter was investigated recently in [1 -3 ]. In this contribution, in addition to outlining the model framework and summarizing the most important findings from[1 -3 ], we report a few new results regarding constraining parameters characterizing the highdensity behavior of nuclear symmetry energy. In particular, the constraints on the pressure of neutron star matter extracted from combining the X-ray observations of the neutron star radius, the minimum-maximum mass M 2.01 M⊙, and causality condition agree very well with those extracted from analyzing the tidal deformability data by the LIGO ＋ Virgo Collaborations. The limitations of using the radius and/or tidal deformability of neutron stars to constrain the high-density nuclear symmetry energy are discussed.

关 键 词：中子星物质 天体物理学 方程 状态 核子 数据提取 调查结果 模型框架 

分 类 号：O571.5[理学—粒子物理与原子核物理]