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Time-domain metric reconstruction for self-force applications

Time-domain metric reconstruction for self-force applications
Time-domain metric reconstruction for self-force applications
We present a new method for calculation of the gravitational self-force (GSF) in Kerr geometry, based on a time-domain reconstruction of the metric perturbation from curvature scalars. In this approach, the GSF is computed directly from a certain scalarlike self-potential that satisfies the time-domain Teukolsky equation on the Kerr background. The approach is computationally much cheaper than existing time-domain methods, which rely on a direct integration of the linearized Einstein’s equations and are impaired by mode instabilities. At the same time, it retains the utility and flexibility of a time-domain treatment, allowing calculations for any type of orbit (including highly eccentric or unbound ones) and the possibility of self-consistently evolving the orbit under the effect of the GSF. Here we formulate our method, and present a first numerical application, for circular geodesic orbits in Schwarzschild geometry. We discuss further applications.
1550-7998
Barack, Leor
f08e66d4-c2f7-4f2f-91b8-f2c4230d0298
Giudice, Paco
83f58b00-e0d2-4932-8c32-1020a3b37c75
Barack, Leor
f08e66d4-c2f7-4f2f-91b8-f2c4230d0298
Giudice, Paco
83f58b00-e0d2-4932-8c32-1020a3b37c75

Barack, Leor and Giudice, Paco (2017) Time-domain metric reconstruction for self-force applications. Physical Review D, 95. (doi:10.1103/PhysRevD.95.104033).

Record type: Article

Abstract

We present a new method for calculation of the gravitational self-force (GSF) in Kerr geometry, based on a time-domain reconstruction of the metric perturbation from curvature scalars. In this approach, the GSF is computed directly from a certain scalarlike self-potential that satisfies the time-domain Teukolsky equation on the Kerr background. The approach is computationally much cheaper than existing time-domain methods, which rely on a direct integration of the linearized Einstein’s equations and are impaired by mode instabilities. At the same time, it retains the utility and flexibility of a time-domain treatment, allowing calculations for any type of orbit (including highly eccentric or unbound ones) and the possibility of self-consistently evolving the orbit under the effect of the GSF. Here we formulate our method, and present a first numerical application, for circular geodesic orbits in Schwarzschild geometry. We discuss further applications.

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Accepted/In Press date: 30 April 2017
e-pub ahead of print date: 24 May 2017

Identifiers

Local EPrints ID: 412262
URI: https://eprints.soton.ac.uk/id/eprint/412262
ISSN: 1550-7998
PURE UUID: 6df1fabf-76c0-480f-8a42-bad97f7d3eaa

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Date deposited: 14 Jul 2017 16:30
Last modified: 13 Mar 2019 19:47

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