Merger and Mass Ejection of Neutron Star Binaries
Merger and Mass Ejection of Neutron Star Binaries
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DOI：
10.1146/annurev-nucl-101918-023625
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发表时间：
2019-08
影响因子：
12.4
通讯作者：
M. Shibata;K. Hotokezaka
中科院分区：
文献类型：
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作者：
M. Shibata;K. Hotokezaka
中子星双子星和黑洞-中子星双子星的合并是地面引力波（GW）探测器最有希望的来源之一，也是高能天体物理现象，正如GW170817事件中对引力波和电磁波（EM）的观测所说明的那样。这些中子星双星的合并也是r过程核合成最有希望的地点。完全广义相对论（Numerical relativity）下的数值模拟是对合并过程、发射的gw、质量抛射过程以及由此产生的EM发射进行理论预测的独特方法。基于最新的数值相对论模拟结果，我们总结了目前对中子星合并和随后的质量抛射过程的理解。我们强调，数值相对论模拟的预测与GW170817的光学和红外观测结果基本一致。
Mergers of binary neutron stars and black hole–neutron star binaries are among the most promising sources for ground-based gravitational-wave (GW) detectors and are also high-energy astrophysical phenomena, as illustrated by the observations of GWs and electromagnetic (EM) waves in the event of GW170817. Mergers of these neutron star binaries are also the most promising sites for r-process nucleosynthesis. Numerical simulation in full general relativity (numerical relativity) is a unique approach to the theoretical prediction of the merger process, GWs emitted, mass ejection process, and resulting EM emission. We summarize the current understanding of the processes of neutron star mergers and subsequent mass ejection based on the results of the latest numerical-relativity simulations. We emphasize that the predictions of the numerical-relativity simulations agree broadly with the optical and IR observations of GW170817.