We have followed the evolution of multi-mass star clusters containing massive central black holes through collisional $N$-body simulations done on GRAPE6. Each cluster is composed of between 16,384 to 131,072 stars together with a black hole with an initial mass of $M_{BH}=1000 M_\odot$. We follow the evolution of the clusters under the combined influence of two-body relaxation, stellar mass-loss and tidal disruption of stars by the massive central black hole. We find that the (3D) mass density profile follows a power-law distribution $\rho \sim r^{-\alpha}$ with slope $\alpha=1.55$ inside the sphere of influence of the central black hole. This leads to a constant density profile of bright stars in projection, which makes it highly unlikely that core collapse clusters contain intermediate-mass black holes. Instead globular clusters containing massive central black holes can be fitted with standard King profiles. Due to energy generation in the cusp, star clusters with intermediate-mass black holes (IMBHs) expand. The cluster expansion is so strong that clusters which start very concentrated can end up among the least dense clusters. The amount of mass segregation in the core is also smaller compared to post-collapse clusters without IMBHs. Most stellar mass black holes with masses $M_{BH}>5 M_\odot$ are lost from the clusters within a few Gyrs through mutual encounters in the cusp around the IMBH. Black holes in star clusters disrupt mainly main-sequence stars and giants and no neutron stars. The disruption rates are too small to form an IMBH out of a $M_{BH} \approx 50$ $M_{BH}$ progenitor black hole even if all material from disrupted stars is accreted onto the black hole, unless star clusters start with central densities significantly higher than what is seen in present day globular clusters.


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