论文标题
动态二进制二进制中子星星合并模拟中的有限温度效应：参数方法的验证
Finite-temperature effects in dynamical-spacetime binary neutron star merger simulations: Validation of the parametric approach
论文作者
论文摘要
状态的参数方程（EOSS）为系统研究中子星合并模拟中的EOS效应提供了重要的工具。在这项工作中，我们对参数计算有限温度的EOS表执行了M*帧的数值验证。 Raithel等人引入的框架。 （2019年），提供了一个模型，用于将任何冷的β-均衡EOS扩展到有限的植物和任意电子分数。在这项工作中，我们对SFHO有限的EOS进行了二元中性星星合并的数值进化，以及同一EOS的M* - approximation，其中近似值使用零温度，beta均衡的sfho sfho sfho sfho sfho，并替换了有限的构图和构图 - 与组合物的零件相互依赖。我们发现，与使用SFHO完整版的结果相比，EOS的大致版本能够准确地重新创建二进制中子星残留的温度和热压轮廓。我们还发现，在两种情况下，合并动力学和重力波信号都符合良好的一致性，〜1-2％的差异通过EOS的近似值引入了合并后重力波峰频率。我们得出结论，可以可靠地用于探测数值模拟中的中子星的合并属性。
Parametric equations of state (EoSs) provide an important tool for systematically studying EoS effects in neutron star merger simulations. In this work, we perform a numerical validation of the M*-framework for parametrically calculating finite-temperature EoS tables. The framework, introduced in Raithel et al. (2019), provides a model for generically extending any cold, beta-equilibrium EoS to finite-temperatures and arbitrary electron fractions. In this work, we perform numerical evolutions of a binary neutron star merger with the SFHo finite-temperature EoS, as well as with the M*-approximation of this same EoS, where the approximation uses the zero-temperature, beta-equilibrium slice of SFHo and replaces the finite-temperature and composition-dependent parts with the M*-model. We find that the approximate version of the EoS is able to accurately recreate the temperature and thermal pressure profiles of the binary neutron star remnant, when compared to the results found using the full version of SFHo. We additionally find that the merger dynamics and gravitational wave signals agree well between both cases, with differences of ~1-2% introduced into the post-merger gravitational wave peak frequencies by the approximations of the EoS. We conclude the M*-framework can be reliably used to probe neutron star merger properties in numerical simulations.
