Black Hole-Neutron Star Binary Merger Calculations: GRB Progenitors and the Stability of Mass Transfer

Details Black Hole-Neutron Star Binary Merger Calculations: GRB Progenitors and the Stability of Mass Transfer Black Hole-Neutron Star Binary Merger Calculations: GRB Progenitors and the Stability of Mass Transfer

2006-05-19

arxiv.org/abs/astro-ph/0605512v1

Astronomy and Astrophysics

Astrophysics

8 pages, 5 figures, in Proceedings of the Albert Einstein Century International Conference, Paris, France, 2005, edited by Jea

Scientific paper

10.1063/1.2399634

We have calculated the first dynamical evolutions of merging black hole-neutron star binaries that treat the combined spacetime in a nonperturbative general relativistic framework. Using the conformal flatness approximation, we have studied how the location of the tidal disruption radius with respect to the the black hole horizon and innermost stable circular orbit (ISCO) affects the qualitative evolution of the system. Based on simple arguments, we show that for a binary mass ratio q>~0.24, tidal disruption occurs outside the ISCO, while the opposite is true for q<~0.24. When tidal disruption occurs sufficiently far outside the ISCO, mass is transferred unstably from the neutron star to the black hole, resulting in the complete disruption of the neutron star. When tidal disruption occurs slightly within the ISCO, we find that some of the mass forms an extremely hot disk around the black hole. The resulting configurations in this case are excellent candidates for the progenitors of short-hard gamma ray bursts.

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