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Title:
Mergers of Black Hole-Neutron Star Binaries. I. Methods and First Results
Authors:
Rantsiou, Emmanouela; Kobayashi, Shiho; Laguna, Pablo; Rasio, Frederic A.
Affiliation:
AA(Department of Physics and Astronomy, Northwestern University, Evanston, IL 60208; , .), AB(Astrophysics Research Institute, Liverpool John Moores University, Twelve Quays House, Egerton Wharf, Birkenhead CH41 1LD, UK; .), AC(Department of Astronomy and Astrophysics and Department of Physics, Pennsylvania State University, University Park, PA 16802;.), AD(Department of Physics and Astronomy, Northwestern University, Evanston, IL 60208; , .)
Publication:
The Astrophysical Journal, Volume 680, Issue 2, pp. 1326-1349. (ApJ Homepage)
Publication Date:
06/2008
Origin:
UCP
ApJ Keywords:
Stars: Binaries: Close, Black Hole Physics, Gamma Rays: Bursts, Relativity, Stars: Neutron
DOI:
10.1086/587858
Bibliographic Code:
2008ApJ...680.1326R

Abstract

We use a 3D relativistic SPH (smoothed particle hydrodynamics) code to study mergers of black hole-neutron star (BH-NS) binary systems with low mass ratios, adopting q≡MNS/MBH~=0.1 as a representative case. The outcome of such mergers depends sensitively on both the magnitude of the BH spin and its obliquity (i.e., the inclination of the binary orbit with respect to the equatorial plane of the BH). In particular, only systems with sufficiently high BH spin parameter a and sufficiently low orbital inclinations allow any NS matter to escape or to form a long-lived disk outside the BH horizon after disruption. Mergers of binaries with orbital inclinations above ~60° lead to complete prompt accretion of the entire NS by the BH, even for the case of an extreme Kerr BH. We find that the formation of a significant disk or torus of NS material around the BH always requires a near-maximal BH spin and a low initial inclination of the NS orbit just prior to merger.
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