A self-dual curvature formulation unifies the Regge-Wheeler-Zerilli and Bardeen-Press-Teukolsky equations on spherical backgrounds as components of one tensorial curvature equation.
Gravitational waveforms from a point particle orbiting a Schwarzschild black hole
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abstract
We numerically solve the inhomogeneous Zerilli-Moncrief and Regge-Wheeler equations in the time domain. We obtain the gravitational waveforms produced by a point-particle of mass $\mu$ traveling around a Schwarzschild black hole of mass M on arbitrary bound and unbound orbits. Fluxes of energy and angular momentum at infinity and the event horizon are also calculated. Results for circular orbits, selected cases of eccentric orbits, and parabolic orbits are presented. The numerical results from the time-domain code indicate that, for all three types of orbital motion, black hole absorption contributes less than 1% of the total flux, so long as the orbital radius r_p(t) satisfies r_p(t)> 5M at all times.
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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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Unifying the Regge-Wheeler-Zerilli and Bardeen-Press-Teukolsky formalisms on spherical backgrounds
A self-dual curvature formulation unifies the Regge-Wheeler-Zerilli and Bardeen-Press-Teukolsky equations on spherical backgrounds as components of one tensorial curvature equation.
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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.