General Relativistic Simulations of Black Hole-Neutron Star Mergers: Effects of Black-Hole Spin

Details General Relativistic Simulations of Black Hole-Neutron Star Mergers: Effects of Black-Hole Spin General Relativistic Simulations of Black Hole-Neutron Star Mergers: Effects of Black-Hole Spin

May 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aps..aprt11007e&link_type=abstract

American Physical Society, 2009 APS April Meeting, May 2-5, 2009, abstract #T11.007

Physics

Scientific paper

Binary black hole-neutron star (BHNS) binary mergers are candidate engines for both short-hard gamma-ray bursts and detectable gravitational radiation. Using our most recent conformal thin-sandwich BHNS initial data and our fully GR hydrodynamics code, which is now AMR-capable, we are able to simulate these binaries accurately through inspiral, merger, and ringdown. We explore the effects of BH spin (aligned and anti-aligned with the orbital angular momentum) by evolving binaries with BH:NS mass ratio q=3 that are nearly identical, except the BH spin is varied between a/MBH=-0.5 (anti-aligned) to 0.75. The number of orbits before merger increases with a/MBH. We also study the nonspinning BH case in depth, varying q between 1, 3, and 5. Gravitational waveforms are calculated and compared to binary BH waveforms. Only a small disk (< 0.01M) forms for the anti-aligned spin case (a/MBH=-0.5) and for the largest mass ratio case (q=5). By contrast, a massive (Mdisk 0.2M), hot disk forms in the rapidly spinning a/MBH=0.75 aligned BH case. Such a disk could drive a SGRB, possibly by, e.g., producing a copious flux of ν-ν pairs.

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