Precisely computing bound orbits of spinning bodies around black holes. II. Generic orbits

In this paper, we continue our study of the motion spinning test bodies orbiting Kerr black holes. Nonspinning follow geodesics spacetime in which they move. A body's spin couples to curvature that spacetime, introducing a ``spin-curvature force'' pushes worldline away from geodesic trajectory. The spin-curvature force is an important example postgeodesic effect must be modeled carefully order accurately characterize One motivation for work understand how include such effects models gravitational waves produced inspiral stellar mass into massive paper's predecessor, describe technique computing bound orbits around holes with frequency-domain description can solved very precisely. present overview methods, as well results are eccentric and nearly equatorial (i.e., orbit's no more than $\mathcal{O}(S)$ out plane). apply formulation fully generic case---orbits inclined eccentric, small arbitrarily oriented. We compute trajectories follow, affects quantities observable orbital frequencies ${\mathrm{\ensuremath{\Omega}}}_{r}$, ${\mathrm{\ensuremath{\Omega}}}_{\ensuremath{\theta}}$ ${\mathrm{\ensuremath{\Omega}}}_{\ensuremath{\phi}}$.