Orbital Evolution of Extreme-Mass-Ratio Black-Hole Binaries with
  Numerical Relativity
  We perform the first fully nonlinear numerical simulations of black-hole
binaries with mass ratios 100:1. Our technique for evolving such extreme mass
ratios is based on the moving puncture approach with a new gauge condition and
an optimal choice of the mesh refinement (plus large computational resources).
We achieve a convergent set of results for simulations starting with a small
nonspinning black hole just outside the ISCO that then performs over two orbits
before plunging into the 100 times more massive black hole. We compute the
gravitational energy and momenta radiated as well as the final remnant
parameters and compare these quantities with the corresponding perturbative
estimates. The results show a close agreement. We briefly discuss the relevance
of this simulations for Advanced LIGO, third-generation ground based detectors,
and LISA observations, and self-force computations.
