Production of EMRIs in Supermassive Black Hole Binaries
  We consider the formation of extreme mass-ratio inspirals (EMRIs) sourced
from a stellar cusp centred on a primary supermassive black hole (SMBH) and
perturbed by an inspiraling less massive secondary SMBH. The problem is
approached numerically, assuming the stars are non-interacting over these short
timescales and performing an ensemble of restricted three-body integrations.
From these simulations we see that not only can EMRIs be produced during this
process, but the dynamics are also quite rich. In particular, most of the EMRIs
are produced through a process akin to the Kozai-Lidov mechanism, but with
strong effects due to the non-Keplerian stellar potential, general relativity,
and non-secular oscillations in the angular momentum on the orbital timescale
of the binary SMBH system.
