标题： 新的{\em 从头计算}约束扩展Skyrme状态方程用于中子星、超新星和双星合并的模拟：I. 低密度区域 显示英文标题

标题： New {\em ab initio} constrained extended Skyrme equations of state for simulations of neutron stars, supernovae and binary mergers: I. Subsaturation density domain

摘要： 在核心坍缩超新星和双中子星合并的数值模拟中，通过外部表格实现关于物质能量和成分的信息，这些表格涵盖了天体物理演化过程中探索的巨大热力学条件范围。 迄今为止，已经贡献了超过120个通用状态方程（EOS）表格。 不幸的是，并非所有表格都符合当前理论和实验核物理以及中子星天体物理观测的约束。 系统研究致密物质性质在这些天体物理现象演化中的作用需要提供更多的EOS表格。 我们构建了一组通用的EOS表格。 在零温度下，它们符合所有目前接受的约束，包括 {\em 从头计算}纯中子物质的手征有效场论计算。 此集合旨在探索有效质量作为密度函数的行为的广泛变化，这反映在广泛的热行为中。 我们采用了通过贝叶斯推理技术生成的布鲁塞尔扩展Skyrme相互作用。 开发了一个扩展的核统计平衡模型，用于建模亚饱和的不均匀核物质（NM）。 在这里，我们研究了亚饱和不均匀NM在广泛密度、温度和质子分数范围内的性质。 我们详细分析了向均匀物质的转变机制并估算了转变密度。 我们的主要结果包括在新中子星内部地壳中存在厚层富含中子的氦或氢同位素，在温暖且富含中子的物质中存在大量奇异的氢和氦同位素，以及对冷恒星物质热力学稳定性的详细研究。 EOS表格可在\textsc{CompOSE}在线数据库中公开获取。 显示英文摘要

摘要： In numerical simulations of core-collapse supernova and binary neutron stars mergers, information about the energetics and composition of matter is implemented via external tables covering the huge ranges of thermodynamic conditions explored during the astrophysical evolution. More than 120 general-purpose equation of state (EOS) tables have been contributed so far. Unfortunately, not all of them comply with current constraints from theoretical and experimental nuclear physics and astrophysical observations of neutron stars. Systematic investigations of the role that dense matter properties play in the evolution of these astrophysical phenomena require that more EOS tables are provided. We build a set of general-purpose EOS tables. At zero temperature, they comply with all currently accepted constraints, including {\em ab initio} chiral effective field theory calculations of pure neutron matter. This set is designed to explore a wide variety of the behaviors of the effective masses as functions of density, which is reflected into a wide range of thermal behaviors. We employ Brussels extended Skyrme interactions generated by means of Bayesian inference techniques. An extended nuclear statistical equilibrium model is developed for modeling sub-saturated inhomogeneous nuclear matter (NM). Here, we study the properties of sub-saturated inhomogeneous NM over wide ranges of density, temperature, and proton fraction. We analyze in detail the mechanisms of transition to homogeneous matter and estimate the transition density. Our key results include a thick layer of neutron rich isotopes of He or H in the inner crusts of neo-neutron stars, significant abundance of exotic isotopes of H and He in warm and neutron-rich matter and a detailed study of the thermodynamic stability of cold stellar matter. The EOS tables are publicly available in the \textsc{CompOSE} online database.