Gravitational radiation from hyperbolic orbits: comparison between self-force, post-Minkowskian, post-Newtonian, and numerical relativity results

Abstract

In this work I use a frequency-domain Regge-Wheeler-Zerilli approach to compute the gravitational wave energy radiated by a compact body moving along a hyperbolic or parabolic geodesic of a Schwarzschild black hole. I compare my results with the latest post-Minkowskian (PM) calculations for the radiated energy and find agreement for hyperbolic orbits with large impact parameters and characterized by a velocity at infinity, $v_{\infty }$, as large as $v_{\infty }/c=0.7$. I also find agreement between my results and the leading-order PM expansion for the radiation absorbed by the black hole. I make further comparisons with post-Newtonian (PN) theory and show the effectiveness of a simple PN-PM hybrid model. Finally, I make a first comparison of the radiated energy between self-force and numerical relativity.

18 pages, 8 figures, 1 table. Updated to match published version

References in corpus (2)

• Enhancing the SEOBNRv5 effective-one-body waveform model with second-order gravitational self-force fluxes
• Spin-up and mass-gain in hyperbolic encounters of spinning black holes

Cited by in corpus (1)

• Resummed energy loss in extreme-mass-ratio scattering using critical orbits