Self-force calculations of radiated gravitational wave energy from hyperbolic orbits around Schwarzschild black holes agree with post-Minkowskian results for large impact parameters and velocities up to 0.7c, with further comparisons to post-Newtonian and numerical relativity.
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EMRI GWB characteristic strain is ~10x higher for black-hole compact objects than neutron-star or white-dwarf cases, with SMBH spin contributing ~1% enhancement and eccentricity negligible after circularization.
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Gravitational radiation from hyperbolic orbits: comparison between self-force, post-Minkowskian, post-Newtonian, and numerical relativity results
Self-force calculations of radiated gravitational wave energy from hyperbolic orbits around Schwarzschild black holes agree with post-Minkowskian results for large impact parameters and velocities up to 0.7c, with further comparisons to post-Newtonian and numerical relativity.
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Gravitational wave background from extreme-mass-ratio inspirals
EMRI GWB characteristic strain is ~10x higher for black-hole compact objects than neutron-star or white-dwarf cases, with SMBH spin contributing ~1% enhancement and eccentricity negligible after circularization.