Cooling Timescale for Protoneutron Stars and Properties of Nuclear Matter: Effective Mass and Symmetry Energy at High Densities
Cooling Timescale for Protoneutron Stars and Properties of Nuclear Matter: Effective Mass and Symmetry Energy at High Densities
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DOI：
10.3847/1538-4357/ab1d4b
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发表时间：
2019-04
期刊：
影响因子：
--
通讯作者：
K. Nakazato;H. Suzuki
中科院分区：
文献类型：
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作者：
K. Nakazato;H. Suzuki
研究了质子中子星（PNS）的冷却过程，重点研究了其对热致密物质性质的敏感性。建立了以两倍饱和密度下的核有效质量和核对称能为控制参数的状态方程，用于系统研究。本文使用的数值代码遵循求解具有中微子扩散的广义相对论恒星结构的PNS的准静态演化。由中微子光曲线计算得到的冷却时间尺度在高密度下有效质量较大、对称能较小的模型更长。本文的结果与其他状态方程的结果进行了比较，发现它们对有效质量和中子星半径的依赖关系是一致的。
The cooling process of a protoneutron star (PNS) is investigated with focus on its sensitivity to properties of hot and dense matter. An equation of state, which includes the nucleon effective mass and nuclear symmetry energy at twice the saturation density as control parameters, is constructed for systematic studies. The numerical code utilized in this study follows a quasi-static evolution of a PNS solving the general-relativistic stellar structure with neutrino diffusion. The cooling timescale evaluated from the neutrino light curve is found to be longer for the models with larger effective masses and smaller symmetry energies at high densities. The present results are compared with those for other equations of state and it is found that they are consistent in terms of their dependences on the effective mass and neutron star radius.