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The evolution of circular, non-equatorial orbits of Kerr black holes due to gravitational-wave emission
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abstract
A major focus of much current research in gravitation theory is on understanding how radiation reaction drives the evolution of a binary system, particularly in the extreme mass ratio limit. Such research is of direct relevance to gravitational-wave sources for space-based detectors (such as LISA). We present here a study of the radiative evolution of circular (i.e., constant Boyer-Lindquist coordinate radius), non-equatorial Kerr black hole orbits. Recent theorems have shown that, at least in an adiabatic evolution, such orbits evolve from one circular configuration into another, changing only their radius and inclination angle. This constrains the system's evolution in such a way that the change in its Carter constant can be deduced from knowledge of gravitational wave fluxes propagating to infinity and down the black hole's horizon. Thus, in this particular case, a local radiation reaction force is not needed. In accordance with post-Newtonian weak-field predictions, we find that inclined orbits radiatively evolve to larger inclination angles (although the post-Newtonian prediction overestimates the rate of this evolution in the strong field by a factor $\lesssim 3$). We also find that the gravitational waveforms emitted by these orbits are rather complicated, particularly when the hole is rapidly spinning, as the radiation is influenced by many harmonics of the orbital frequencies.
Forward citations
Cited by 13 Pith papers
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Modified Teukolsky Formalism for Extreme Mass-Ratio Inspirals in Higher-Derivative Gravity
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Efficient and Stable Computation of Gravitational-Wave Fluxes from Generic Kerr Orbits via a Unified HeunC Framework
A unified confluent HeunC framework with hybrid connection-coefficient computation and adaptive bi-power quadrature yields relative errors of order 10^{-11} and 2-10x speedups over existing packages for total radiativ...
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Resonant interactions from dynamical perturbers on generic orbits around an extreme mass ratio inspiral
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Extreme mass-ratio inspiral within an ultralight scalar cloud I. Scalar radiation
Scalar radiation from an EMRI in an ultralight scalar cloud is computed semi-analytically, showing dipole clouds decelerate and quadrupole clouds accelerate the inspiral, with up to about 100 rad dephasing after 18 months.
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4.5PN and 2SF calculations of gravitational energy flux for quasicircular compact binaries agree.
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