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The inspiral of a stellar mass compact object falling into a massive Kerrblack hole can be broken into three different regimes: An adiabatic inspiralphase, where the inspiral timescale is much larger than the orbital period; alate-time radial infall, which can be approximated as a plunging geodesic; anda regime where the body transitions from the inspiral to plunge. In earlierwork, Ori and Thorne have outlined a method to compute the trajectory duringthis transition for a compact object in a circular, equatorial orbit. Wegeneralize this technique to include inclination and eccentricity.

The transition from adiabatic inspiral to geodesic plunge for a compact object around a massive Kerr black hole: Generic orbits