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Covariant perturbations of Schwarzschild black holes

Chris A Clarkson et al 2003 Class. Quantum Grav. 20 3855-3884   doi: 10.1088/0264-9381/20/18/301  Help

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Chris A Clarkson1 and Richard K Barrett2
1 Relativity and Cosmology Group, Department of Mathematics and Applied Mathematics, University of Cape Town, Rondebosch 7701, Cape Town, South Africa
2 Astronomy and Astrophysics Group, Department of Physics and Astronomy, University of Glasgow, University Avenue, Glasgow G12 8QQ, UK
E-mail: clarkson@maths.uct.ac.za and richard@astro.gla.ac.uk

Abstract. We present a new covariant and gauge-invariant perturbation formalism for dealing with spacetimes having spherical symmetry (or some preferred spatial direction) in the background, and apply it to the case of gravitational wave propagation in a Schwarzschild black-hole spacetime. The 1 + 3 covariant approach is extended to a '1 + 1 + 2 covariant sheet' formalism by introducing a radial unit vector in addition to the timelike congruence, and decomposing all covariant quantities with respect to this. The background Schwarzschild solution is discussed and a covariant characterization is given. We give the full first-order system of linearized 1 + 1 + 2 covariant equations, and we show how, by introducing (time and spherical) harmonic functions, these may be reduced to a system of first-order ordinary differential equations and algebraic constraints for the 1 + 1 + 2 variables which may be solved straightforwardly. We show how both odd- and even-parity perturbations may be unified by the discovery of a covariant, frame- and gauge-invariant, transverse-traceless tensor describing gravitational waves, which satisfies a covariant wave equation equivalent to the Regge–Wheeler equation for both even- and odd-parity perturbations. We show how the Zerilli equation may be derived from this tensor, and derive a similar transverse-traceless tensor equation equivalent to this equation. The so-called special quasinormal modes with purely imaginary frequency emerge naturally. The significance of the degrees of freedom in the choice of the two frame vectors is discussed, and we demonstrate that, for a certain frame choice, the underlying dynamics is governed purely by the Regge–Wheeler tensor. The two transverse-traceless Weyl tensors which carry the curvature of gravitational waves are discussed, and we give the closed system of four first-order ordinary differential equations describing their propagation. Finally, we consider the extension of this work to the study of gravitational waves in other astrophysical situations.

PACS numbers: 04.25.Mx, 04.30.−w, 04.20.−q, 04.20.Cv, 04.70.−s, 97.60.Lf

Print publication: Issue 18 (21 September 2003)
Received 28 October 2002, in final form 19 June 2003
Published 20 August 2003

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