Kavli Affiliate: Scott A. Hughes
| First 5 Authors: Lisa V. Drummond, Alexandra G. Hanselman, Devin R. Becker, Scott A. Hughes,
| Summary:
The study of spinning bodies moving in curved spacetime has relevance to
binary black hole systems with large mass ratios, as well as being of formal
interest. At zeroth order in a binary’s mass ratio, the smaller body moves on a
geodesic of the larger body’s spacetime. Post-geodesic corrections describing
forces driving the small body’s worldline away from geodesics must be
incorporated to model the system accurately. An important post-geodesic effect
is the gravitational self-force, which describes the small body’s interaction
with its own spacetime curvature. This effect includes the backreaction due to
gravitational-wave emission that leads to the inspiral of the small body into
the black hole. When a spinning body orbits a black hole, its spin couples to
spacetime curvature. This introduces another post-geodesic correction known as
the spin-curvature force. An osculating geodesic integrator that includes both
the backreaction due to gravitational waves and spin-curvature forces can be
used to generate a spinning-body inspiral. In this paper, we use an osculating
geodesic integrator to combine the leading backreaction of gravitational waves
with the spin-curvature force. Our analysis only includes the leading
orbit-averaged dissipative backreaction, and examines the spin-curvature force
to leading order in the small body’s spin. This is sufficient to build generic
inspirals of spinning bodies, and serves as a foundation for further work
examining how to include secondary spin in large-mass-ratio waveform models.
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