The coalescence remnant of spinning binary black holes

Details The coalescence remnant of spinning binary black holes The coalescence remnant of spinning binary black holes

2003-05-15

arxiv.org/abs/astro-ph/0305287v2

Phys.Rev. D69 (2004) 027505

Astronomy and Astrophysics

Astrophysics

4 pages, 5 figures

Scientific paper

10.1103/PhysRevD.69.027505

We compute the gravitational radiation generated in the evolution of a family of close binary black hole configurations, using a combination of numerical and perturbative approximation methods. We evolve the binaries with spins, $s$, aligned or counter-aligned with the orbital angular momentum from near the innermost stable circular orbit (ISCO) down to the final single rotating black hole. For the moderately spinning holes studied here the remnant Kerr black hole formed at the end of an inspiral process have a rotation parameter $a/M\approx0.72+0.32(s/m_H)$, suggesting it is difficult (though not excluded) to end up with near maximally rotating holes from such scenarios.

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