Abstract
The mass of stellar black holes (BHs) is currently thought to be in the 3-20 Msun range, but is highly uncertain: recent observations indicate the existence of at least one BH with mass >20 Msun. The metallicity of the progenitor star strongly influences the mass of the remnant, as only metal-poor stars can have a final mass higher than ~40 Msun, and are expected to directly collapse into BHs with mass >25 Msun. By means of N-body simulations, we investigate the formation and evolution of massive stellar BHs (MSBHs, with mass >25 Msun) in young dense star clusters. We study the effects of MSBHs on the population of X-ray sources.
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