论文标题
对称能量对状态方程的影响，以模拟核心折叠超新星和中子星合并
Effects of symmetry energy on equation of state for simulations of core-collapse supernovae and neutron-star mergers
论文作者
论文摘要
我们基于具有较小的对称能量斜率$ l $的扩展相对论均值场模型，构建了一个新的状态方程（EOS），以用于核心偏转超新星和中子星合并的数值模拟，这与实验性核数据兼容了近期的中子星。基于$ L = 40 $ MEV的扩展TM1（TM1E）模型的新EOS表（EOS4）以相同的表格形式设计，并与常用的Shen EOS（EOS2）相比，基于原始TM1模型，其$ L = 110.8 $ MEV。这对于进行数值模拟并检查对称能量及其对天体物理现象的密度依赖性的影响是方便且有用的。与EOS2中使用的TM1模型相比，TM1E模型提供了类似的最大中子星质量，但半径较小，并且对于$ 1.4 m_ \ odot $中子星，它与当前约束更一致。通过比较EOS4和EOS2之间的相图和热力学数量，发现TM1E模型预测了富含中子的物质的非均匀物质和柔软的EOS区域。在低质子分数的情况下，观察到EOS4和EOS2之间的显着差异，而对称物质的性质保持不变。
We construct a new equation of state (EOS) for numerical simulations of core-collapse supernovae and neutron-star mergers based on an extended relativistic mean-field model with a small symmetry energy slope $L$, which is compatible with both experimental nuclear data and recent observations of neutron stars. The new EOS table (EOS4) based on the extended TM1 (TM1e) model with $L=40$ MeV is designed in the same tabular form and compared with the commonly used Shen EOS (EOS2) based on the original TM1 model with $L=110.8$ MeV. This is convenient and useful for performing numerical simulations and examining the influences of symmetry energy and its density dependence on astrophysical phenomena. In comparison with the TM1 model used in EOS2, the TM1e model provides a similar maximum neutron-star mass but smaller radius and tidal deformability for a $1.4 M_\odot$ neutron star, which is more consistent with current constraints. By comparing the phase diagram and thermodynamic quantities between EOS4 and EOS2, it is found that the TM1e model predicts relatively larger region of nonuniform matter and softer EOS for neutron-rich matter. Significant differences between EOS4 and EOS2 are observed in the case with low proton fraction, while the properties of symmetric matter remain unchanged.
