GW170817, general relativistic magnetohydrodynamic simulations, and the neutron star maximum mass

被引：372

作者：

Ruiz, Milton ^{[1
]}

Shapiro, Stuart L. ^{[1
,2
,3
]}

Tsokaros, Antonios ^{[1
]}

机构：

[1] Univ Illinois, Dept Phys, Urbana, IL 61801 USA

[2] Univ Illinois, Dept Astron, Urbana, IL 61801 USA

[3] Univ Illinois, NCSA, Urbana, IL 61801 USA

来源：

PHYSICAL REVIEW D | 2018年 / 97卷 / 02期

基金：

美国国家科学基金会;

关键词：

GAMMA-RAY BURSTS; EQUATION-OF-STATE; ACCRETION FLOWS; HOST GALAXY; AFTERGLOW; ELECTRODYNAMICS; STABILITY; ROTATION; INERTIA; MOMENT;

D O I：

10.1103/PhysRevD.97.021501

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

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.

引用

页数：6

共 90 条

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