Coalescence of Black Hole-Neutron Star Binaries.
We review the current status of general relativistic studies for the coalescence of black hole-neutron star (BH-NS) binaries. First, procedures for a solution of BH-NS binaries in quasi-equilibrium circular orbits and the numerical results, such as quasi-equilibrium sequence and mass-shedding limit, of the high-precision computation, are summarized. Then, the current status of numerical-relativity simulations for the merger of BH-NS binaries is described. We summarize our understanding for the merger and/or tidal disruption processes, the criterion for tidal disruption, the properties of the remnant formed after the tidal disruption, gravitational waveform, and gravitational-wave spectrum.
Yukawa Institute for Theoretical Physics, Kyoto University, Kyoto, 606-8502 Japan.
Masaru
M
Shibata
Graduate School of Arts and Sciences, The University of Tokyo, Tokyo, 153-8902 Japan.
Keisuke
K
Taniguchi