Resonantly enhanced and diminished strong-field gravitational-wave
  fluxes
  The inspiral of a stellar mass ($1 - 100\,M_\odot$) compact body into a
massive ($10^5 - 10^7\,M_\odot$) black hole has been a focus of much effort,
both for the promise of such systems as astrophysical sources of gravitational
waves, and because they are a clean limit of the general relativistic two-body
problem. Our understanding of this problem has advanced significantly in recent
years, with much progress in modeling the "self force" arising from the small
body's interaction with its own spacetime deformation. Recent work has shown
that this self interaction is especially interesting when the frequencies
associated with the orbit's $\theta$ and $r$ motions are in an integer ratio:
$\Omega_\theta/\Omega_r = \beta_\theta/\beta_r$, with $\beta_\theta$ and
$\beta_r$ both integers. In this paper, we show that key aspects of the self
interaction for such "resonant" orbits can be understood with a relatively
simple Teukolsky-equation-based calculation of gravitational-wave fluxes. We
show that fluxes from resonant orbits depend on the relative phase of radial
and angular motions. The purpose of this paper is to illustrate in simple terms
how this phase dependence arises using tools that are good for strong-field
orbits, and to present a first study of how strongly the fluxes vary as a
function of this phase and other orbital parameters. Future work will use the
full dissipative self force to examine resonant and near resonant strong-field
effects in greater depth, which will be needed to characterize how a binary
evolves through orbital resonances.
