The role of the supermassive black hole spin in the estimation of the
  EMRI event rate
  A common result to all EMRI investigations on rates is that the possibility
that a compact object merges with the MBH after only one intense burst of GWs
is much more likely than a slow adiabatic inspiral, an EMRI. The later is
referred to as a "plunge" because the compact object dives into the MBH. The
event rates for plunges are orders of magnitude larger than slow inspirals. On
the other hand, nature MBH's are most likely Kerr and the magnitude of the spin
has been sized up to be high. We calculate the number of periapsis passages
that a compact object set on to an extremely radial orbit goes through before
being actually swallowed by the Kerr MBH and we then translate it into an event
rate for a LISA-like observatory, such as the proposed ESA mission eLISA/NGO.
We prove that a "plunging" compact object is conceptually indistinguishable
from an adiabatic, slow inspiral; plunges spend on average up to hundred of
thousands of cycles in the bandwidth of the detector for a two years mission.
This has an important impact on the event rate, enhancing in some cases
significantly, depending on the spin of the MBH and the inclination. Moreover,
it has been recently proved that the production of low-eccentricity EMRIs is
severely blocked by the presence of a blockade in the rate at which orbital
angular momenta change takes place. This is the result of relativistic
precession on to the stellar potential torques and hence affects EMRIs
originating via resonant relaxation at distances of about $\sim 10^{-2}$ pc
from the MBH. Since high-eccentricity EMRIs are a result of two-body
relaxation, they are not affected by this phenomenon. Therefore we predict that
eLISA EMRI event rates will be dominated by high-eccentricity binaries, as we
present here.
