Speaker
Description
We analyze about a thousand globular cluster (GC) models simulated using the MOCCA Monte Carlo code for star cluster evolution to study black hole - black hole interactions in these dense stellar sys- tems that can lead to gravitational wave emission. We extracted information for all coalescing binary black holes (BBHs) that merge via gravitational ra- diation from these GC models and for those BHs that collide due to 2-body, 3-body and 4-body dy- namical interactions. By obtaining results from a substantial number of realistic star clusters evolu- tion models, that cover different initial parameters (masses, metallicities, densities etc) we have an ex- tremely large statistical sample of two black holes which merge or collide within a Hubble time. We found that creation of an Intermediate Mass Black Hole (IMBH, defined as a BH with mass above 100 M ) in a GC’s center has large influence on merger and collision rates.
