Abstract
We compute the conservative piece of the gravitational self-force (GSF) acting on a particle of mass as it moves along an (unstable) circular geodesic orbit between the innermost stable orbit and the light ring of a Schwarzschild black hole of mass . More precisely, we construct the function (related to Detweiler’s gauge-invariant “redshift” variable), where is the regularized metric perturbation in the Lorenz gauge, is the four-velocity of in the background Schwarzschild metric of , and is an invariant coordinate constructed from the orbital frequency . In particular, we explore the behavior of just outside the “light ring” at (i.e., ), where the circular orbit becomes null. Using the recently discovered link between and the piece , linear in the symmetric mass ratio , of the main radial potential of the effective-one-body (EOB) formalism, we compute from our GSF data the EOB function over the entire domain (thereby extending previous results limited to ). We find that diverges like at the light-ring limit, , explain the physical origin of this divergent behavior, and discuss its consequences for the EOB formalism. We construct accurate global analytic fits for , valid on the entire domain (and possibly beyond), and give accurate numerical estimates of the values of and its first three derivatives at the innermost stable circular orbit , as well as the associated shift in the frequency of that orbit. In previous work we used GSF data on slightly eccentric orbits to compute a certain linear combination of and its first two derivatives, involving also the piece of a second EOB radial potential . Combining these results with our present global analytic representation of , we numerically compute on the interval .
1 More- Received 5 September 2012
DOI:https://doi.org/10.1103/PhysRevD.86.104041
© 2012 American Physical Society