Coalescence of black hole-neutron star binaries

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.

Automated summary

The current status of general relativistic studies on the coalescences of black hole-neutron star binaries is reviewed, highlighting high-precision computations in quasiequilibrium circular orbits and numerical-relativity simulations for the merger process. Understanding of tidal disruption, properties of merger remnant and ejected material, gravitational waveforms, gravitational-wave spectra, and expected electromagnetic counterparts to black hole-neutron star coalescences are summarized.