The last orbit of binary black holes

Details The last orbit of binary black holes The last orbit of binary black holes

2006-01-23

arxiv.org/abs/gr-qc/0601091v1

Phys.Rev.D73:061501,2006

Astronomy and Astrophysics

Astrophysics

General Relativity and Quantum Cosmology

5 pages, 5 figures, revtex4

Scientific paper

10.1103/PhysRevD.73.061501

We have used our new technique for fully numerical evolutions of orbiting black-hole binaries without excision to model the last orbit and merger of an equal-mass black-hole system. We track the trajectories of the individual apparent horizons and find that the binary completed approximately one and a third orbits before forming a common horizon. Upon calculating the complete gravitational radiation waveform, horizon mass, and spin, we find that the binary radiated 3.2% of its mass and 24% of its angular momentum. The early part of the waveform, after a relatively short initial burst of spurious radiation, is oscillatory with increasing amplitude and frequency, as expected from orbital motion. The waveform then transitions to a typical `plunge' waveform; i.e. a rapid rise in amplitude followed by quasinormal ringing. The plunge part of the waveform is remarkably similar to the waveform from the previously studied `ISCO' configuration. We anticipate that the plunge waveform, when starting from quasicircular orbits, has a generic shape that is essentially independent of the initial separation of the binary.

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