Selfforce on a scalar charge in Kerr spacetime: Eccentric equatorial orbits
Abstract
We present a numerical code for calculating the selfforce 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. DPRVDAQ15507998 78, 084021 (2008)10.1103/PhysRevD.78.084021], in conjunction with modesum regularization. Our work is part of a program to develop a computational architecture for fast and efficient selfforce calculations, alternative to timedomain methods. We find that our frequencydomain method outperforms existing timedomain 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 scalarfield selfforce 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 selfforce tangent to the fourvelocity.
 Publication:

Physical Review D
 Pub Date:
 June 2011
 DOI:
 10.1103/PhysRevD.83.124038
 arXiv:
 arXiv:1103.0287
 Bibcode:
 2011PhRvD..83l4038W
 Keywords:

 04.25.Nx;
 04.25.g;
 04.70.Bw;
 PostNewtonian approximation;
 perturbation theory;
 related approximations;
 Approximation methods;
 equations of motion;
 Classical black holes;
 General Relativity and Quantum Cosmology;
 Astrophysics  High Energy Astrophysical Phenomena
 EPrint:
 26 pages, 9 figures. Minor typo corrected