Coalescence of Black Hole-Neutron Star Binaries

doi:doi:10.12942/lrr-2011-6

url: http://www.livingreviews.org/lrr-2011-6

doi: 10.12942/lrr-2011-6

Living Rev. Relativity 14 (2011), 6

Coalescence of Black Hole-Neutron Star Binaries

Masaru Shibata and Keisuke Taniguchi

Affiliation(s)

¹ Yukawa Institute for Theoretical Physics, Kyoto University, Kyoto 606-8502, Japan
² Graduate School of Arts and Sciences, The University of Tokyo, Tokyo 153-8902, Japan

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Article 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.

Keywords: gravitational waves, neutron star, black hole, numerical relativity

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Since a Living Reviews in Relativity article may evolve over time, please cite the access <date>, which uniquely identifies the version of the article you are referring to:

Masaru Shibata and Keisuke Taniguchi,
"Coalescence of Black Hole-Neutron Star Binaries",
Living Rev. Relativity 14, (2011), 6. URL (cited on <date>):
http://www.livingreviews.org/lrr-2011-6

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