Self-force on extreme mass ratio inspirals via curved spacetime effective field theory

Details Self-force on extreme mass ratio inspirals via curved spacetime effective field theory Self-force on extreme mass ratio inspirals via curved spacetime effective field theory

2008-01-07

arxiv.org/abs/0801.0900v2

Phys.Rev.D79:064002,2009

Astronomy and Astrophysics

Astrophysics

General Relativity and Quantum Cosmology

22 pages, 5 figures; references added, revised Appendices B & C, corrected typos, revisions throughout for clarification parti

Scientific paper

10.1103/PhysRevD.79.064002

In this series we construct an effective field theory (EFT) in curved spacetime to study gravitational radiation and backreaction effects. We begin in this paper with a derivation of the self-force on a compact object moving in the background spacetime of a supermassive black hole. The EFT approach utilizes the disparity between two length scales, which in this problem are the size of the compact object and the radius of curvature of the background spacetime, to treat the orbital dynamics of the compact object, described as an effective point particle, separately from its tidal deformations. Ultraviolet divergences are regularized using Hadamard's {\it partie finie} to isolate the non-local finite part from the quasi-local divergent part. The latter is constructed from a momentum space representation for the graviton retarded propagator and is evaluated using dimensional regularization in which only logarithmic divergences are relevant for renormalizing the parameters of the theory. As a first important application of this framework we explicitly derive the first order self-force given by Mino, Sasaki, Tanaka, Quinn and Wald. Going beyond the point particle approximation, to account for the finite size of the object, we demonstrate that for extreme mass ratio inspirals the motion of a compact object is affected by tidally induced moments at $O(\epsilon^4)$, in the form of an Effacement Principle. The relatively large radius-to-mass ratio of a white dwarf star allows for these effects to be enhanced until the white dwarf becomes tidally disrupted, a potentially $O(\epsilon^2)$ process, or plunges into the supermassive black hole. This work provides a new foundation for further exploration of higher order self force corrections, gravitational radiation and spinning compact objects.

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