Coalescence of Black Hole–Neutron Star Binaries

Masaru Shibata  
Yukawa Institute for Theoretical Physics, Kyoto University
Kyoto 606-8502, Japan

'External link'http://www2.yukawa.kyoto-u.ac.jp/~mshibata/
and
Keisuke Taniguchi  
Graduate School of Arts and Sciences, The University of Tokyo
Tokyo 153-8902, Japan

Abstract

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.


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