期刊
ASTROPHYSICAL JOURNAL
卷 680, 期 2, 页码 1326-1349出版社
IOP PUBLISHING LTD
DOI: 10.1086/587858
关键词
binaries : close; black hole physics; gamma rays : bursts; relativity; stars : neutron
资金
- Science and Technology Facilities Council [PP/E001149/1] Funding Source: researchfish
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 M-NS/M-BH similar or equal to 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 similar to 60 degrees 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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