GW170817, general relativistic magnetohydrodynamic simulations, and the neutron star maximum mass
GW170817, general relativistic magnetohydrodynamic simulations, and the neutron star maximum mass
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DOI：
10.1103/physrevd.97.021501
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发表时间：
2018-01-11
影响因子：
5
通讯作者：
Tsokaros, Antonios
中科院分区：
文献类型：
--
作者：
Ruiz, Milton;Shapiro, Stuart L.;Tsokaros, Antonios
最近在广义相对论磁流体力学(GRMHD)中的数值模拟为解释GW170817发现提供了有用的约束。将观测数据与这些模拟相结合，得出了冷的球形中子星的最大质量(tov极限)的界限：m-max(Sph)小于或类似于2.74/β，其中β是均匀旋转的中子星的最大质量(超极大极限)与非自转星的最大质量的比率。因果关系的论点允许Beta高达1.27，而大多数现实的候选状态方程预测Beta更接近1.2，得出M-max(Sph)在2.16-2.28m(圆点)的范围内。基于这些模拟的最小假设集将这一分析与之前的分析区分开来，但导致了类似的估计。然而，有一些警告，它们被列举和讨论。这些警告可以通过进一步的模拟和分析来消除，以巩固基本论点。
Recent numerical simulations in general relativistic magnetohydrodynamics (GRMHD) provide useful constraints for the interpretation of the GW170817 discovery. Combining the observed data with these simulations leads to a bound on the maximum mass of a cold, spherical neutron star (the TOV limit): M-max(sph) less than or similar to 2.74/beta, where beta is the ratio of the maximum mass of a uniformly rotating neutron star (the supramassive limit) over the maximum mass of a nonrotating star. Causality arguments allow beta to be as high as 1.27, while most realistic candidate equations of state predict beta to be closer to 1.2, yielding M-max(sph) in the range 2.16-2.28M(circle dot). A minimal set of assumptions based on these simulations distinguishes this analysis from previous ones, but leads a to similar estimate. There are caveats, however, and they are enumerated and discussed. The caveats can be removed by further simulations and analysis to firm up the basic argument.