Akcay, S., Dempsey, D. and Dolan, S.R. orcid.org/0000-0002-4672-6523 (2017) Spin–orbit precession for eccentric black hole binaries at first order in the mass ratio. Classical and Quantum Gravity, 34 (8). 084001. ISSN 0264-9381
Abstract
We consider spin–orbit ('geodetic') precession for a compact binary in strong-field gravity. Specifically, we compute ψ, the ratio of the accumulated spin-precession and orbital angles over one radial period, for a spinning compact body of mass m 1 and spin s 1, with ${{s}_{1}}\ll Gm_{1}^{2}/c$ , orbiting a non-rotating black hole. We show that ψ can be computed for eccentric orbits in both the gravitational self-force and post-Newtonian frameworks, and that the results appear to be consistent. We present a post-Newtonian expansion for ψ at next-to-next-to-leading order, and a Lorenz-gauge gravitational self-force calculation for ψ at first order in the mass ratio. The latter provides new numerical data in the strong-field regime to inform the effective one-body model of the gravitational two-body problem. We conclude that ψ complements the Detweiler redshift z as a key invariant quantity characterizing eccentric orbits in the gravitational two-body problem.
Metadata
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Copyright, Publisher and Additional Information: | © 2017 IOP Publishing Ltd. This is an author produced version of a paper subsequently published in Classical and Quantum Gravity. Uploaded in accordance with the publisher's self-archiving policy. | ||||||
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Institution: | The University of Sheffield | ||||||
Academic Units: | The University of Sheffield > Faculty of Science (Sheffield) > School of Mathematics and Statistics (Sheffield) | ||||||
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Depositing User: | Symplectic Sheffield | ||||||
Date Deposited: | 30 Mar 2017 09:07 | ||||||
Last Modified: | 20 Mar 2018 01:38 | ||||||
Published Version: | https://doi.org/10.1088/1361-6382/aa61d6 | ||||||
Status: | Published | ||||||
Publisher: | IOP Publishing | ||||||
Refereed: | Yes | ||||||
Identification Number: | https://doi.org/10.1088/1361-6382/aa61d6 |