  We present preliminary results from self-consistent, high resolution direct
{\it N}-body simulations of massive black hole binaries in mergers of galactic
nuclei. The dynamics of the black hole binary includes the full Post-Newtonian
corrections (up to 2.5PN) to its equations of motion. We show that massive
black holes starting at separations of 100 pc can evolve down to
gravitational-wave-induced coalescence in less than a Hubble time. The
binaries, in our models, often form with very high eccentricity and, as a
result, reach separations of 50 Schwarzschild radius with eccentricities which
are clearly distinct from zero -- even though gravitational wave emission damps
the eccentricity during the inspiral. These deviations from exact circular
orbits, at such small separations, may have important consequences for LISA
data analysis.
