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

By A. Buonanno, Yanbei Chen, T. Damour. 2005

169 citations recorded by the source corpus.

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{sup 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 describingmore » the gravitational-wave signal emitted by the entire process of coalescence of precessing binaries of spinning black holes.« less

Subfields: Astronomy and Astrophysics, Ocean Engineering

View Paper: https://www.semanticscholar.org/paper/2108c5767a9d303a439cc4a124907f87d7a1f288

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In Astronomy and Astrophysics

1. T. Damour
2. S. Naoz
3. B. Kocsis
4. G. Schāfer
5. P. Jaranowski
6. N. Yunes
7. Abraham Loeb
8. Rafael A. Porto

In Ocean Engineering

1. N. Yunes
2. P. Jaranowski
3. G. Schāfer
4. T. Damour
5. Rafael A. Porto
6. E. Poisson

Citations in the corpus

• Effective one body approach to the dynamics of two spinning black holes with next-to-leading order spin-orbit coupling (2008, methodology): “This method was the first to provide estimates of the complete waveform (covering inspiral, plunge, merger, and ring-down) of a coalescing black hole binary, both for non-spinning systems [3], and for spinning ones [5].”
• RESONANT POST-NEWTONIAN ECCENTRICITY EXCITATION IN HIERARCHICAL THREE-BODY SYSTEMS (2012, methodology): “The Hamiltonian is then (e.g., Buonanno et al. 2006): H2body1PN =− (m31 +m 3 2)p 4 8c2m31m 3 2 − k 2(3m21 + 7m1m2 + 3m 2 2)p 2 2c2m1m2r − k 2(p · r)2 2c2r3 + k4(m1 +m2) 2µ 2c2r2 , where r is the radius vector between the two bodies, with magnitude r, the linear momentum of the effective one body…”