论文标题
中子恒星灵感和聚结的天体物理含义
Astrophysical Implications of Neutron Star Inspiral and Coalescence
论文作者
论文摘要
在引力波中观察到的两个中子星的第一个灵感非常接近，从而使这种同时的引力波和电磁观察发现已经预期了几年。他们的合并，然后在电磁望远镜的光谱带上观察到伽马射线爆发和基洛诺瓦。这些GW和电磁观测导致了理解短伽马射线爆发的巨大进步。确定最重的元素的起源；并确定中子星的最大质量。从引力波形上的潮汐的烙印以及X射线二进制的观察结果，可以提取灵感中子星的半径和可变形性。半径，最大质量和因果关系共同限制了状态的中子星程，未来的约束可能来自于合并后振荡的观察结果。我们有选择地回顾这些结果，并用衍生和估计填充一些物理学。
The first inspiral of two neutron stars observed in gravitational waves was remarkably close, allowing the kind of simultaneous gravitational wave and electromagnetic observation that had not been expected for several years. Their merger, followed by a gamma-ray burst and a kilonova, was observed across the spectral bands of electromagnetic telescopes. These GW and electromagnetic observations have led to dramatic advances in understanding short gamma-ray bursts; determining the origin of the heaviest elements; and determining the maximum mass of neutron stars. From the imprint of tides on the gravitational waveforms and from observations of X-ray binaries, one can extract the radius and deformability of inspiraling neutron stars. Together, the radius, maximum mass, and causality constrain the neutron-star equation of state, and future constraints can come from observations of post-merger oscillations. We selectively review these results, filling in some of the physics with derivations and estimates.
