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In this paper, we study the formation and dynamical evolution of blackhole-black hole (BH-BH) binaries in young star clusters (YSCs), by means ofN-body simulations. The simulations include metallicity-dependent recipes forstellar evolution and stellar winds, and have been run for three differentmetallicities (Z = 0.01, 0.1 and 1 Zsun). Following recent theoretical modelsof wind mass-loss and core-collapse supernovae, we assume that the mass of thestellar remnants depends on the metallicity of the progenitor stars. We findthat BH-BH binaries form efficiently because of dynamical exchanges: in oursimulations, we find about 10 times more BH-BH binaries than double neutronstar binaries. The simulated BH-BH binaries form earlier in metal-poor YSCs,which host more massive black holes (BHs) than in metal-rich YSCs. Thesimulated BH-BH binaries have very large chirp masses (up to 80 Msun), becausethe BH mass is assumed to depend on metallicity, and because BHs can grow inmass due to the merger with stars. The simulated BH-BH binaries span a widerange of orbital periods (10^-3-10^7 yr), and only a small fraction of them(0.3 per cent) is expected to merge within a Hubble time. We discuss theestimated merger rate from our simulations and the implications for AdvancedVIRGO and LIGO.

Dynamics of stellar black holes in young star clusters with different metallicities - II. Black hole-black hole binaries