Finite-temperature effects in dynamical spacetime binary neutron star merger simulations: validation of the parametric approach
Finite-temperature effects in dynamical spacetime binary neutron star merger simulations: validation of the parametric approach
复制标题
动态时空双中子星合并模拟中的有限温度效应：参数方法的验证
DOI：
10.1093/mnras/stac2450
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发表时间：
2022
影响因子：
4.8
通讯作者：
Paschalidis, Vasileios
中科院分区：
文献类型：
--
作者：
Raithel, Carolyn A.;Espino, Pedro;Paschalidis, Vasileios
参量状态方程（EoS）是系统研究中子星星合并模拟中EoS效应的重要工具。在这项工作中，我们进行了数值验证theM*-框架参数计算有限温度EoS表。Raithel等人提出的框架，提供了一个模型，一般扩展任何冷，β平衡EoS有限的温度和任意的电子分数。在这项工作中，我们进行了一个双中子星星合并与SFHo有限温度EoS的数值演化，以及与M *-近似相同的EoS，其中近似使用SFHo的零温度，β-平衡切片，并用M *-模型取代有限温度和成分相关的部分。我们发现，近似版本的EoS是能够准确地重建的温度和热的压力分布的二进制中子星星残留物相比，发现使用完整版本的SFHO的结果。我们还发现，合并动力学和引力波信号在这两种情况下吻合得很好，差异为$\lesssim 1\！-\！2\，{\textrm{ %}}$引入到合并后的引力波峰值频率的近似的EoS。我们的结论是，M *-框架可以可靠地用于探测中子星星合并的性质在数值模拟。
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 theM*-framework for parametrically calculating finite-temperature EoS tables. The framework, introduced by Raithel et al., provides a model for generically extending any cold, β-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 theM*-approximation of this same EoS, where the approximation uses the zero-temperature, β-equilibrium slice of SFHo and replaces the finite-temperature and composition-dependent parts with theM*-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 $\lesssim 1\!-\!2\,{\textrm{per cent}}$ introduced into the post-merger gravitational wave peak frequencies by the approximations of the EoS. We conclude that theM*-framework can be reliably used to probe neutron star merger properties in numerical simulations.