The last orbit of binary black holes
| dc.creator | Campanelli, M. | |
| dc.creator | Lousto, C. O. | |
| dc.creator | Zlochower, Y. | |
| dc.date | 2006-01-23 | |
| dc.date.accessioned | 2026-07-07T10:28:14Z | |
| dc.date.available | 2026-07-07T10:28:14Z | |
| dc.description | 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. | |
| dc.description | 5 pages, 5 figures, revtex4 | |
| dc.identifier | https://arxiv.org/abs/gr-qc/0601091 | |
| dc.identifier | http://arxiv.org/abs/gr-qc/0601091 | |
| dc.identifier | Phys.Rev.D73:061501,2006 | |
| dc.identifier | doi:10.1103/PhysRevD.73.061501 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/177379 | |
| dc.subject | General Relativity and Quantum Cosmology | |
| dc.title | The last orbit of binary black holes | |
| dc.type | text |