A dynamical gravitational wave source in a dense cluster
  Making use of a new N-body model to describe the evolution of a moderate-size
globular cluster we investigate the characteristics of the population of black
holes within such a cluster. This model reaches core-collapse and achieves a
peak central density typical of the dense globular clusters of the Milky Way.
Within this high-density environment we see direct confirmation of the merging
of two stellar remnant black-holes in a dynamically-formed binary, a
gravitational wave source. We describe how the formation, evolution and
ultimate ejection/destruction of binary systems containing black holes impacts
the evolution of the cluster core. Also, through comparison with previous
models of lower density, we show that the period distribution of black hole
binaries formed through dynamical interactions in this high-density model
favours the production of gravitational wave sources. We confirm that the
number of black holes remaining in a star cluster at late times and the
characteristics of the binary black hole population depend on the nature of the
star cluster, critically on the number density of stars and by extension the
relaxation timescale.
