Reconstruction of black hole metric perturbations from the Weyl curvature
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 t...
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2002
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| Acceso en línea: | https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_05562821_v66_n2_p_Lousto http://hdl.handle.net/20.500.12110/paper_05562821_v66_n2_p_Lousto |
| Aporte de: |
| Sumario: | 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. © 2002 The American Physical Society. |
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