Transition from inspiral to plunge in precessing binaries of spinning black holes

被引:193
作者
Buonanno, Alessandra [1 ]
Chen, Yanbei
Damour, Thibault
机构
[1] Univ Paris 07, CEA, Observ Paris, CNRS,UMR 7164, F-75221 Paris 05, France
[2] Albert Einstein Inst, Max Planck Inst Gravitat Phys, D-14476 Golm, Germany
[3] Inst Hautes Etud Sci, F-91440 Bures Sur Yvette, France
[4] APC, F-75005 Paris, France
关键词
D O I
10.1103/PhysRevD.74.104005
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
We investigate the nonadiabatic dynamics of spinning black-hole binaries by using an analytical Hamiltonian completed with a radiation-reaction force, containing spin couplings, which matches the known rates of energy and angular-momentum losses on quasicircular orbits. We consider both a straightforward post-Newtonian-expanded Hamiltonian (including spin-dependent terms), and a version of the resummed post-Newtonian Hamiltonian defined by the effective one-body approach. We focus on the influence spin terms have on the dynamics and waveforms. We evaluate the energy and angular momentum released during the final stage of inspiral and plunge. For an equal-mass binary the energy released between 40 Hz and the frequency beyond which our analytical treatment becomes unreliable is found to be, when using the effective one-body dynamics, 0.6%M for antialigned maximally spinning black holes, 5%M for aligned maximally spinning black holes, and 1.8%M for nonspinning configurations. In confirmation of previous results, we find that, for all binaries considered, the dimensionless rotation parameter J/E-2 is always smaller than unity at the end of the inspiral, so that a Kerr black hole can form right after the inspiral phase. By matching a quasinormal mode ring down to the last reliable stages of the plunge, we construct complete waveforms approximately describing the gravitational-wave signal emitted by the entire process of coalescence of precessing binaries of spinning black holes.
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页数:26
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