Simulating neutron stars with a flexible enthalpy-based equation of state parametrization in spectre
Simulating neutron stars with a flexible enthalpy-based equation of state parametrization in spectre
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DOI：
10.1103/physrevd.107.123017
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发表时间：
2023-01
影响因子：
5
通讯作者：
I. Legred;Yoonsoo Kim;N. Deppe;K. Chatziioannou;F. Foucart;F. H'ebert;Lawrence E. Kidder
中科院分区：
文献类型：
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作者：
I. Legred;Yoonsoo Kim;N. Deppe;K. Chatziioannou;F. Foucart;F. H'ebert;Lawrence E. Kidder
中子星合并的数值模拟代表了解释多信使观测的全部复杂性和限制超核物质性质的关键一步。目前，模拟受到一系列因素的限制，包括计算性能和输入物理不确定性，如中子星状态方程。在这项工作中，我们通过引入一种新的基于相对论热焓的冷的β平衡物质的解析参数化，有效地扩展了可用于模拟的核唯象的范围。结果表明，新的EMPH参数化能捕捉到包括强相变在内的一系列核行为。我们在Texttt{SPECTRE}程序中实现了焓参数化，模拟了孤立的中子星，并与常用的谱参数化和多变参数化的性能进行了比较。我们发现，对于用这两种方法中的任何一种都能很好地表示的核模型，例如简单的强子EOSS，其计算性能是相当的。我们发现，焓参数化进一步允许我们模拟更复杂的强子模型或具有相变的模型，这是目前的参数化所不能达到的。
Numerical simulations of neutron star mergers represent an essential step toward interpreting the full complexity of multimessenger observations and constraining the properties of supranuclear matter. Currently, simulations are limited by an array of factors, including computational performance and input physics uncertainties, such as the neutron star equation of state. In this work, we expand the range of nuclear phenomenology efficiently available to simulations by introducing a new analytic parametrization of cold, beta-equilibrated matter that is based on the relativistic enthalpy. We show that the new \emph{enthalpy parametrization} can capture a range of nuclear behavior, including strong phase transitions. We implement the enthalpy parametrization in the \texttt{SpECTRE} code, simulate isolated neutron stars, and compare performance to the commonly used spectral and polytropic parametrizations. We find comparable computational performance for nuclear models that are well represented by either parametrization, such as simple hadronic EoSs. We show that the enthalpy parametrization further allows us to simulate more complicated hadronic models or models with phase transitions that are inaccessible to current parametrizations.