Merger and Mass Ejection of Neutron Star Binaries

被引：198

作者：

Shibata, Masaru ^{[1
,2
]}

Hotokezaka, Kenta ^{[3
]}

机构：

[1] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-14476 Potsdam, Germany

[2] Kyoto Univ, Yukawa Inst Theoret Phys, Ctr Gravitat Phys, Kyoto 6068502, Japan

[3] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA

来源：

ANNUAL REVIEW OF NUCLEAR AND PARTICLE SCIENCE, VOL 69 | 2019年 / 69卷

基金：

日本学术振兴会;

关键词：

neutron star merger; black hole; neutron star; gravitational waves; electromagnetic counterparts; r-process nucleosynthesis; R-PROCESS NUCLEOSYNTHESIS; COOLED ACCRETION DISKS; BLACK-HOLE; GRAVITATIONAL-WAVES; RADIOACTIVE DECAY; DRIVEN WINDS; GAMMA-RAYS; KILONOVA; GW170817; EMISSION;

D O I：

10.1146/annurev-nucl-101918-023625

中图分类号：

O57 [原子核物理学、高能物理学];

学科分类号：

070202 ;

摘要：

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.

引用

页码：41 / 64

页数：24

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