Adiabatic evolution due to the conservative scalar self-force during orbital resonances

Abstract

We calculate the scalar self-force experienced by a scalar point-charge orbiting a Kerr black hole along $rθ$-resonant geodesics. We use the self-force to calculate the averaged rate of change of the charge's orbital energy $\langle\dot{E}\rangle$, angular momentum $\langle\dot{L}_z\rangle$, and Carter constant $\langle\dot{Q}\rangle$, which together capture the leading-order adiabatic, secular evolution of the point-charge. Away from resonances, only the dissipative (time anti-symmetric) components of the self-force contribute to $\langle\dot{E}\rangle$, $\langle\dot{L}_z\rangle$, and $\langle\dot{Q}\rangle$. We demonstrate, using a new numerical code, that during $rθ$ resonances conservative (time symmetric) scalar perturbations also contribute to $\langle\dot{Q}\rangle$ and, thus, help drive the adiabatic evolution of the orbit. Furthermore, we observe that the relative impact of these conservative contributions to $\langle\dot{Q}\rangle$ is particularly strong for eccentric 2:3 resonances. These results provide the first conclusive numerical evidence that conservative scalar perturbations of Kerr spacetime are non-integrable during $rθ$ resonances.