Equation of state of nuclear matter and neutron stars: Quark mean-field model versus relativistic mean-field model

被引:4
|
作者
Zhu, Zhenyu [1 ]
Li, Ang [2 ]
Hu, Jinniu [3 ]
Shen, Hong [3 ]
机构
[1] Shanghai Jiao Tong Univ, Tsung Dao Lee Inst, Shanghai 201210, Peoples R China
[2] Xiamen Univ, Dept Astron, Xiamen 361005, Peoples R China
[3] Nankai Univ, Sch Phys, Tianjin 300071, Peoples R China
基金
中国国家自然科学基金; 中国博士后科学基金;
关键词
GRAVITATIONAL-WAVE SOURCE; BAYESIAN-INFERENCE; ELECTROMAGNETIC COUNTERPART; MAXIMUM MASS; GW170817; CONSTRAINTS; KILONOVA; NICER; SELECTION; BILBY;
D O I
10.1103/PhysRevC.108.025809
中图分类号
O57 [原子核物理学、高能物理学];
学科分类号
070202 ;
摘要
The equation of state of neutron-rich nuclear matter is of interest to both nuclear physics and astrophysics. We have demonstrated the consistency between laboratory and astrophysical nuclear matter in neutron stars by considering low-density nuclear physics constraints (from 208Pb neutron-skin thickness) and high-density astrophysical constraints (from neutron star global properties). We have used both quark-level and hadron-level models, taking the quark mean-field (QMF) model and the relativistic mean-field (RMF) model as examples, respectively. We have constrained the equation of states of neutron stars and some key nuclear matter parameters within the Bayesian statistical approach, using the first multimessenger event GW170817/AT 2017gfo, as well as the mass-radius simultaneous measurements of PSR J0030+0451 and PSR J0740+6620 from NICER, and the neutron-skin thickness of 208Pb from both PREX-II measurement and ab initio calculations. Our results show that, compared with the RMF model, the QMF model's direct coupling of quarks with mesons and gluons leads to the evolution of the in-medium nucleon mass with the quark mass correction. This feature enables the QMF model a wider range of model applicability, as shown by a slow drop of the nucleon mass with density and a large value at saturation that is jointly constrained by nuclear physics and astronomy.
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页数:13
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