Modeling the horizon-absorbed gravitational flux for equatorial-circular orbits in Kerr spacetime
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Author(s)
Taracchini, Andrea
Buonanno, Alessandra
Khanna, Gaurav
Hughes, Scott A
Date Issued
August 2013
Journal
Physical Review D
Publisher
American Physical Society
Citation
Taracchini, Andrea, Alessandra Buonanno, Scott A. Hughes, and Gaurav Khanna. “Modeling the horizon-absorbed gravitational flux for equatorial-circular orbits in Kerr spacetime.” Physical Review D 88, no. 4 (August 2013). © 2013 American Physical Society
Version
Final published version
Abstract
We propose an improved analytical model for the horizon-absorbed gravitational-wave energy flux of a small body in circular orbit in the equatorial plane of a Kerr black hole. Post-Newtonian (PN) theory provides an analytical description of the multipolar components of the absorption flux through Taylor expansions in the orbital frequency. Building on previous work, we construct a mode-by-mode factorization of the absorbed flux whose Taylor expansion agrees with current PN results. This factorized form significantly improves the agreement with numerical results obtained with a frequency-domain Teukolsky code, which evolves through a sequence of circular orbits up to the photon orbit. We perform the comparison between model and numerical data for dimensionless Kerr spins -0.99≤q≤0.99 and for frequencies up to the light ring of the Kerr black hole. Our proposed model enforces the presence of a zero in the flux at an orbital frequency equal to the frequency of the horizon, as predicted by perturbation theory. It also reproduces the expected divergence of the flux close to the light ring. Neither of these features are captured by the Taylor-expanded PN flux. Our proposed absorption flux can also help improve models for the inspiral, merger, ringdown of small mass-ratio binary systems.
MIT Department
Massachusetts Institute of Technology. Department of Physics
MIT Kavli Institute for Astrophysics and Space Research
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DOI of Published Version
https://doi.org/10.1103/PhysRevD.88.044001
