Vol. 14 (2011) > lrr-2011-6

doi: 10.12942/lrr-2011-6
Living Rev. Relativity 14 (2011), 6

Coalescence of Black Hole-Neutron Star Binaries

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

Full text: HTML | PDF (5130.6 Kb)

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

Article Downloads

Article Format Size (Kb)
RIS UTF-8 Latin-1
EndNote UTF-8 Latin-1

Article Citation

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>):

Article History

ORIGINAL http://www.livingreviews.org/lrr-2011-6
Title Coalescence of Black Hole-Neutron Star Binaries
Author Masaru Shibata / Keisuke Taniguchi
Date accepted 7 July 2011, published 29 August 2011
  • Bookmark this article:
  • bibsonomy
  • citeulike
  • delicious
  • digg
  • mendeley
Comment(s) on this article



Impact Factor 2014