The Equation of State of Hot, Dense Matter and Neutron Stars
The Equation of State of Hot, Dense Matter and Neutron Stars
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DOI：
10.1016/j.physrep.2015.12.005
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发表时间：
2015-12
期刊：
影响因子：
--
通讯作者：
J. Lattimer;M. Prakash
中科院分区：
文献类型：
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作者：
J. Lattimer;M. Prakash
纯中子物质理论和核物质对称能实验的最新发展，加上最近对大质量中子星的测量，现在允许对致密物质的状态方程进行相对严格的约束。我们回顾这些约束是如何制定和描述它们对中子星和核心坍缩超新星的影响。我们还研究了致密物质的热性质，这对超新星和中子星星合并是很重要的，但在这个时候不能通过实验来约束。此外，我们考虑了状态方程在中能重离子碰撞中的作用。
Recent developments in the theory of pure neutron matter and experiments concerning the symmetry energy of nuclear matter, coupled with recent measurements of high-mass neutron stars, now allow for relatively tight constraints on the equation of state of dense matter. We review how these constraints are formulated and describe the implications they have for neutron stars and core-collapse supernovae. We also examine thermal properties of dense matter, which are important for supernovae and neutron star mergers, but which cannot be nearly as well constrained at this time by experiment. In addition, we consider the role of the equation of state in medium-energy heavy-ion collisions.