Coalescence remnant of spinning binary black holes
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/m_{H}), suggesting it is difficult (though not excluded) to end up with near maximally rotating holes from such scenarios.
 Publication:

Physical Review D
 Pub Date:
 January 2004
 DOI:
 10.1103/PhysRevD.69.027505
 arXiv:
 arXiv:astroph/0305287
 Bibcode:
 2004PhRvD..69b7505B
 Keywords:

 04.25.Dm;
 04.25.Nx;
 04.30.Db;
 04.70.Bw;
 Numerical relativity;
 PostNewtonian approximation;
 perturbation theory;
 related approximations;
 Wave generation and sources;
 Classical black holes;
 Astrophysics;
 General Relativity and Quantum Cosmology
 EPrint:
 4 pages, 5 figures