论文标题
热超级中子恒星物质的状态方程
Equation of state for hot hyperonic neutron star matter
论文作者
论文摘要
FSU2H方程式模型最初开发用于用Hyperonic核心描述冷中子恒星物质，扩展到有限的温度。结果介绍了广泛的温度和轻子部分，这些温度涵盖了原子恒星物质，中子恒星合并和超新星爆炸的条件。已经发现，当考虑到超声波自由度时，温度对热力学观察物的影响和中子星核的组成更强。对热指数的温度和密度依赖性的评估导致观察到，所谓的$γ$定律（广泛用于中子星级合并模拟）不适合重现真正的热效应，特别是当超音素开始在中子恒星中很丰富时。为了使状态的有限温度方程式易于访问，提供了核酸和超声波$β$稳定的无中微子物质的热指数的简单参数化。
The FSU2H equation-of-state model, originally developed to describe cold neutron star matter with hyperonic cores, is extended to finite temperature. Results are presented for a wide range of temperatures and lepton fractions, which cover the conditions met in protoneutron star matter, neutron star mergers and supernova explosions. It is found that the temperature effects on the thermodynamical observables and the composition of the neutron star core are stronger when the hyperonic degrees of freedom are considered. An evaluation of the temperature and density dependence of the thermal index leads to the observation that the so-called $Γ$ law, widely used in neutron star merger simulations, is not appropriate to reproduce the true thermal effects, specially when hyperons start to be abundant in the neutron star core. To make finite temperature equations of state easily accessible, simple parameterizations of the thermal index for nucleonic and hyperonic $β$-stable neutrino-free matter are provided.
