Self-force on a scalar charge in Kerr spacetime: Eccentric equatorial orbits

Niels Warburton and Leor Barack
Phys. Rev. D 83, 124038 – Published 22 June 2011

Abstract

We present a numerical code for calculating the self-force on a scalar charge moving in a bound (eccentric) geodesic in the equatorial plane of a Kerr black hole. We work in the frequency domain and make use of the method of extended homogeneous solutions [Phys. Rev. D 78, 084021 (2008)], in conjunction with mode-sum regularization. Our work is part of a program to develop a computational architecture for fast and efficient self-force calculations, alternative to time-domain methods. We find that our frequency-domain method outperforms existing time-domain schemes for small eccentricities, and, remarkably, remains competitive up to eccentricities as high as 0.7. As an application of our code, we (i) compute the conservative scalar-field self-force correction to the innermost stable circular equatorial orbit, as a function of the Kerr spin parameter; and (ii) calculate the variation in the rest mass of the scalar particle along the orbit, caused by the component of the self-force tangent to the four-velocity.

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  • Received 1 March 2011

DOI:https://doi.org/10.1103/PhysRevD.83.124038

© 2011 American Physical Society

Authors & Affiliations

Niels Warburton and Leor Barack

  • School of Mathematics, University of Southampton, Southampton SO17 1BJ, United Kingdom

See Also

Self-force on a scalar charge in Kerr spacetime: Circular equatorial orbits

Niels Warburton and Leor Barack
Phys. Rev. D 81, 084039 (2010)

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Vol. 83, Iss. 12 — 15 June 2011

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