  A compact body in orbit about a black hole loses orbital energy and angular
momentum through radiation-reaction processes, inspiralling towards the black
hole until a final plunge. Here we consider a scenario with a charged compact
body in which fluxes of electromagnetic radiation drive this inspiral. We
calculate trajectories in the $(p,e)$ plane for inspirals in the equatorial
plane of a rotating black hole within the adiabatic
(orbital-averaged-dissipative) approximation. We make comparisons with a
non-relativistic Keplerian approximation based on the Abraham-Lorentz force
law, and with standard gravitational-wave driven scenarios. We find that
EM-driven inspirals are less efficiently circularized (i.e. orbits remain more
eccentric at the point of plunge) than their gravitational counterparts, and we
quantify the effect of black hole spin.
