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Late-time decay of gravitational and electromagnetic perturbations along the event horizon

Late-time decay of gravitational and electromagnetic perturbations along the event horizon
Late-time decay of gravitational and electromagnetic perturbations along the event horizon
We study analytically, via the Newman-Penrose formalism, the late-time decay of linear electromagnetic and gravitational perturbations along the event horizon (EH) of black holes. We first analyze in detail the case of a Schwarzschild black hole. Using a straightforward local analysis near the EH, we show that, generically, the “ingoing” (s>0) component of the perturbing field dies off along the EH more rapidly than its “outgoing” (s<0) counterpart. Thus, while along r=const>2M lines both components of the perturbation admit the well-known t-2l-3 decay rate, one finds that along the EH the s<0 component dies off in advanced time v as v-2l-3, whereas the s>0 component dies off as v-2l-4. We then describe the extension of this analysis to a Kerr black hole. We conclude that for axially symmetric modes the situation is analogous to the Schwarzschild case. However, for non-axially symmetric modes both s>0 and s<0 fields decay at the same rate (unlike in the Schwarzschild case).
1550-7998
16pp
Barack, Leor
f08e66d4-c2f7-4f2f-91b8-f2c4230d0298
Ori, Amos
a7e1cc9a-5d14-4e4e-bc3f-6eab0d2f9d64
Barack, Leor
f08e66d4-c2f7-4f2f-91b8-f2c4230d0298
Ori, Amos
a7e1cc9a-5d14-4e4e-bc3f-6eab0d2f9d64

Barack, Leor and Ori, Amos (1999) Late-time decay of gravitational and electromagnetic perturbations along the event horizon. Physical Review D, 60 (124005), 16pp. (doi:10.1103/PhysRevD.60.124005).

Record type: Article

Abstract

We study analytically, via the Newman-Penrose formalism, the late-time decay of linear electromagnetic and gravitational perturbations along the event horizon (EH) of black holes. We first analyze in detail the case of a Schwarzschild black hole. Using a straightforward local analysis near the EH, we show that, generically, the “ingoing” (s>0) component of the perturbing field dies off along the EH more rapidly than its “outgoing” (s<0) counterpart. Thus, while along r=const>2M lines both components of the perturbation admit the well-known t-2l-3 decay rate, one finds that along the EH the s<0 component dies off in advanced time v as v-2l-3, whereas the s>0 component dies off as v-2l-4. We then describe the extension of this analysis to a Kerr black hole. We conclude that for axially symmetric modes the situation is analogous to the Schwarzschild case. However, for non-axially symmetric modes both s>0 and s<0 fields decay at the same rate (unlike in the Schwarzschild case).

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Published date: December 1999

Identifiers

Local EPrints ID: 48004
URI: http://eprints.soton.ac.uk/id/eprint/48004
ISSN: 1550-7998
PURE UUID: 35862476-662c-409d-b602-b0f68851a559
ORCID for Leor Barack: ORCID iD orcid.org/0000-0003-4742-9413

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Date deposited: 20 Aug 2007
Last modified: 17 Dec 2019 01:47

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