Coalescence of black hole–neutron star binaries

Living Reviews in Relativity

Masaru Shibata¹  Koutarou Kyutoku²  Keisuke Taniguchi³ 

[1] Center for Gravitational Physics, Yukawa Institute for Theoretical Physics, Kyoto University, 606-8502, Kyoto, Japan;Max Planck Institute for Gravitational Physics (Albert Einstein Institute), Am Mühlenberg 1, 14476, Potsdam-Golm, Germany;Department of Physics, Kyoto University, 606-8502, Kyoto, Japan;Center for Gravitational Physics, Yukawa Institute for Theoretical Physics, Kyoto University, 606-8502, Kyoto, Japan;Interdisciplinary Theoretical and Mathematical Sciences Program (iTHEMS), RIKEN, 351-0198, Wako, Saitama, Japan;Department of Physics, University of the Ryukyus, 903-0213, Nishihara, Okinawa, Japan;

关键词: Numerical relativity;    Black holes;    Neutron stars;    Gravitational waves;    Gamma-ray burst;    Nucleosynthesis;   

DOI  :  10.1007/s41114-021-00033-4

来源: Springer

【 摘 要 】

We review the current status of general relativistic studies for coalescences of black hole–neutron star binaries. First, high-precision computations of black hole–neutron star binaries in quasiequilibrium circular orbits are summarized, focusing on the quasiequilibrium sequences and the mass-shedding limit. Next, the current status of numerical-relativity simulations for the merger of black hole–neutron star binaries is described. We summarize our understanding for the merger process, tidal disruption and its criterion, properties of the merger remnant and ejected material, gravitational waveforms, and gravitational-wave spectra. We also discuss expected electromagnetic counterparts to black hole–neutron star coalescences.

【 授权许可】

CC BY