Coalescence of black hole--neutron star binaries

TL;DR

This paper reviews the latest computational and simulation studies on black hole--neutron star binary coalescences, focusing on the merger process, gravitational waves, and electromagnetic signals.

Contribution

It provides a comprehensive overview of high-precision quasiequilibrium calculations and numerical relativity simulations for black hole--neutron star mergers, highlighting recent advances.

Findings

Detailed quasiequilibrium sequences and mass-shedding limits

Insights into merger dynamics and tidal disruption

Predictions of gravitational waveforms and electromagnetic counterparts

Abstract

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.