Phys. Rev. D 58, 084019 (1998) [5 pages]Imposition of Cauchy data to the Teukolsky equation. III. The rotating caseSee Also: Erratum Received 18 March 1998; published 11 September 1998 We solve the problem of expressing the Weyl scalars ψ that describe gravitational perturbations of a Kerr black hole in terms of Cauchy data. To do so we use geometrical identities (such as the Gauss-Codazzi relations) as well as the Einstein equations. We are able to explicitly express ψ and ∂tψ as functions only of the extrinsic curvature and the three-metric (and geometrical objects built out of it) of a generic spacelike slice of the spacetime. These results provide the link between initial data and ψ to be evolved by the Teukolsky equation, and can be used to compute the gravitational radiation generated by two orbiting black holes in the close limit approximation. They can also be used to extract wave forms from numerically generated spacetimes. © 1998 The American Physical Society URL:
http://link.aps.org/doi/10.1103/PhysRevD.58.084019
DOI:
10.1103/PhysRevD.58.084019
PACS:
04.30.Db, 04.70.Bw
See AlsoErratum: Manuela Campanelli, Carlos O. Lousto, John Baker, Gaurav Khanna, and Jorge Pullin, Erratum: Imposition of Cauchy data to the Teukolsky equation. III. The rotating case [Phys. Rev. D 58, 084019 (1998)], Phys. Rev. D 62, 069901 (2000). See Also: Manuela Campanelli and Carlos O. Lousto, Imposition of Cauchy data to the Teukolsky equation. I. The nonrotating case, Phys. Rev. D 58, 024015 (1998). |
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