English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Plus monthly

Global: Zendy Tools annual

Global: Zendy Tools monthly

Global: Zendy Free Plan

The study of spinning bodies moving in curved spacetime has relevance tobinary black hole systems with large mass ratios, as well as being of formalinterest. At zeroth order in a binary's mass ratio, the smaller body moves on ageodesic of the larger body's spacetime. Post-geodesic corrections describingforces driving the small body's worldline away from geodesics must beincorporated to model the system accurately. An important post-geodesic effectis the gravitational self-force, which describes the small body's interactionwith its own spacetime curvature. This effect includes the backreaction due togravitational-wave emission that leads to the inspiral of the small body intothe black hole. When a spinning body orbits a black hole, its spin couples tospacetime curvature. This introduces another post-geodesic correction known asthe spin-curvature force. An osculating geodesic integrator that includes boththe backreaction due to gravitational waves and spin-curvature forces can beused to generate a spinning-body inspiral. In this paper, we use an osculatinggeodesic integrator to combine the leading backreaction of gravitational waveswith the spin-curvature force. Our analysis only includes the leadingorbit-averaged dissipative backreaction, and examines the spin-curvature forceto leading order in the small body's spin. This is sufficient to build genericinspirals of spinning bodies, and serves as a foundation for further workexamining how to include secondary spin in large-mass-ratio waveform models.

Extreme mass-ratio inspiral of a spinning body into a Kerr black hole I: Evolution along generic trajectories