Coalescence remnant of spinning binary black holes

Authors

J Baker
M. Campanelli
C. O. Lousto
R. Takahashi

Document Type

Article

Publication Date

2004

Abstract

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 counteraligned with the orbital angular momentum from near the innermost stable circular orbit down to the final single rotating black hole. For the moderately spinning holes studied here the remnant Kerr black holes formed at the end of an inspiral process have rotation parameters a/M≈0.72+0.32(s/mH), suggesting it is difficult (though not excluded) to end up with near maximally rotating holes from such scenarios.

Comments

©2004 American Physical Society

Recommended Citation

Baker, J., et al. "Coalescence remnant of spinning binary black holes." Physical Review D 69.2 (2004): 027505. https://doi.org/10.1103/PhysRevD.69.027505

Publication Title

Physical Review D

DOI

10.1103/PhysRevD.69.027505