Black hole binary dynamics

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 = 2.4 × 10 ⁵ particles are obtained showing systematic eccentricity growth until the relativistic regime is reached, with subsequent coalescence in some cases. This revised version was published online in August 2006 with corrections to the Cover Date.