  We discuss a new N-body simulation method for studying black hole binary
dynamics. This method avoids previous numerical problems due to large mass
ratios and trapped orbits with short periods. A treatment of relativistic
effects is included when the associated time-scale becomes small. Preliminary
results with up to N = 240 000 particles are obtained showing systematic
eccentricity growth until the relativistic regime is reached, with subsequent
coalescence in some cases.
