Phases of Dense Matter in Supernovae and Neutron Stars

被引：0

作者：

Shen Hong ^{[1
]}

Wang Yannan ^{[1
]}

机构：

[1] Nankai Univ, Sch Phys, Tianjin 300071, Peoples R China

来源：

PLASMA SCIENCE & TECHNOLOGY | 2012年 / 14卷 / 07期

基金：

中国国家自然科学基金;

关键词：

relativistic mean-field theory; equation of state; supernova; neutron star; EQUATION-OF-STATE; MEAN-FIELD-THEORY; UNSTABLE NUCLEI; HYPERNUCLEI;

D O I：

10.1088/1009-0630/14/7/03

中图分类号：

O35 [流体力学]; O53 [等离子体物理学];

学科分类号：

070204 ; 080103 ; 080704 ;

摘要：

We study the properties of dense matter at finite temperature with various proton fractions for use in supernova simulations. The relativistic mean-field theory is used to describe homogeneous nuclear matter, while the Thomas-Fermi approximation is adopted to describe inhomogeneous matter. We also discuss the equation of state of neutron star matter at zero temperature in a wide density range. The equation of state at high densities can be significantly softened by the inclusion of hyperons.

引用

页码：581 / 584

页数：4

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