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Phys. Rev. Lett. 83, 3581–3584 (1999)

Inspiraling Black Holes: The Close Limit

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Gaurav Khanna1, John Baker1,2, Reinaldo J. Gleiser3, Pablo Laguna4, Carlos O. Nicasio3, Hans-Peter Nollert5, Richard Price6, and Jorge Pullin1
1Center for Gravitational Physics and Geometry, Department of Physics, The Pennsylvania State University, 104 Davey Lab, University Park, Pennsylvania 16802
2Max-Planck-Institut für Gravitationsphysik, Albert-Einstein-Institut, Am Mühlenberg 1, D-14476 Golm, Germany
3Facultad de Matemática, Astronomía y Física, Universidad Nacional de Córdoba, Ciudad Universitaria, 5000 Cordoba, Argentina
4Department of Astronomy and Astrophysics, The Pennsylvania State University, 525 Davey Lab, University Park, Pennsylvania 16802
5Theoretische Astrophysik, Universität Tübingen, 72076, Tübingen, Germany
6Department of Physics, University of Utah, Salt Lake City, Utah 84112

Received 21 May 1999; published in the issue dated 1 November 1999

We calculate an estimate of the gravitational radiation emitted when two equal mass black holes coalesce at the end of their binary inspiral, using several approximations based on considering the holes close to each other. A shortcoming of our method is that it is limited to models forming final holes with slow rotation, but our results clearly suggest a trend for larger angular momenta. We find that about 1% of the mass energy of the pair will emerge as gravitational waves during the final stages of the collision and that a negligible fraction of the angular momentum will be radiated.

© 1999 The American Physical Society

URL:
http://link.aps.org/doi/10.1103/PhysRevLett.83.3581
DOI:
10.1103/PhysRevLett.83.3581
PACS:
04.30.Db, 04.25.Dm, 04.70.Bw, 97.80.Fk
 
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