原中子星的物态方程
Equation of State for Proto-Neutron Star
摘要：
原中子星（PNS）物态方程（EoS）物理学研究的是有限温度下宽密度范围内富中子物质的性质。本文在球Wigner-Setiz近似的相对论平均场模型中讨论了PNS内壳的结构，以及在由核子和原子核组成的非理想气体维里膨胀中PNS中中微子球周围物质的组成。我们接着讨论了几个新的完整的PNS和超新星的EoS，其详细的组成是重要的中微子动力学。我们着重讨论了不同EoS的一个重要区别--对称能E 'sym的密度依赖性，它与中子星半径的有趣关系，以及丰中子核中中子分布的性质。通过对富中子核中子分布的地面实验、从头算方法的基准计算以及对高质量观测数据的统计分析，加深对E'sym的理解，将促进我们对EoS的认识。
英文摘要：
Physics of the Equation of State (EoS) for proto-neutron star (PNS) concerns properties of neutron rich matter at finite temperature over wide range of densities. In this contribution we discuss the structure of PNS inner crust in a relativisitc mean filed model with spherical Wigner-Setiz approximation, and the composition of matter around neutrino-sphere in PNS in a virial expansion of non-ideal gas composed of nucleons and nuclei. We go on to discuss several new complete EoS for PNS and supernova, whose detailed composition is important for the neutrino dynamics. We focus on one important distinction for various EoS - the density dependence of symmetry energy E'sym, and its interesting correlation with the radii of neutron star, as well as properties of neutron distribution in neutron rich nuclei. Improved understanding of E'sym from terrestrial experiment on neutron distribution of neutron rich nuclei, benchmark calculations via ab initio methods, and statistical analysis on good quality observational data will advance our knowledge on EoS.
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