Reconstruction of black hole metric perturbations from the Weyl curvature

Carlos O. Lousto and Bernard F. Whiting
Phys. Rev. D 66, 024026 – Published 18 July 2002
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Abstract

Perturbation theory of rotating black holes is usually described in terms of Weyl scalars ψ4 and ψ0, which each satisfy Teukolsky’s complex master wave equation and respectively represent outgoing and ingoing radiation. On the other hand metric perturbations of a Kerr hole can be described in terms of (Hertz-like) potentials Ψ in outgoing or ingoing radiation gauges. In this paper we relate these potentials to what one actually computes in perturbation theory, i.e. ψ4 and ψ0. We explicitly construct these relations in the nonrotating limit, preparatory to devising a corresponding approach for building up the perturbed spacetime of a rotating black hole. We discuss the application of our procedure to second order perturbation theory and to the study of radiation reaction effects for a particle orbiting a massive black hole.

  • Received 18 March 2002

DOI:https://doi.org/10.1103/PhysRevD.66.024026

©2002 American Physical Society

Authors & Affiliations

Carlos O. Lousto

  • Department of Physics and Astronomy, University of Texas at Brownsville, Brownsville, Texas 78520
  • Instituto de Astronomía y Física del Espacio–CONICET, Buenos Aires, Argentina

Bernard F. Whiting

  • Department of Physics, P.O. Box 118440, University of Florida, Gainesville, Florida 32611-8440

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Vol. 66, Iss. 2 — 15 July 2002

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