Ruiz Milton, Shapiro Stuart L, Tsokaros Antonios
Department of Physics, University of Illinois at Urbana-Champaign, Urbana, Illinois 61801, USA.
Department of Astronomy and NCSA, University of Illinois at Urbana-Champaign, Urbana, Illinois 61801, USA.
Phys Rev D. 2018 Jan 15;97(2). doi: 10.1103/PhysRevD.97.021501. Epub 2018 Jan 11.
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): , where 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 to be as high as 1.27, while most realistic candidate equations of state predict to be closer to 1.2, yielding in the range 2.16-2.28. 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.
近期广义相对论磁流体动力学（GRMHD）中的数值模拟为GW170817发现的解释提供了有用的限制。将观测数据与这些模拟相结合，得出了冷球形中子星最大质量的界限（TOV极限）： ，其中 是均匀旋转中子星的最大质量（超质量极限）与非旋转恒星最大质量的比值。因果论证允许 高达1.27，而大多数现实的候选状态方程预测 更接近1.2，得出 在2.16 - 2.28范围内。基于这些模拟的一组最小假设使该分析有别于先前的分析，但得出了类似的估计。然而，存在一些警告，在此进行了列举和讨论。通过进一步的模拟和分析可以消除这些警告，以巩固基本论点。
