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Most stars form in dense stellar environments. It is speculated that somedense star clusters may host intermediate-mass black holes (IMBHs), which mayhave formed from runaway collisions between high-mass stars, or from themergers of less massive black holes. Here, we numerically explore the evolutionof populations of planets in star clusters with an IMBH. We study the dynamicalevolution of single-planet systems and free-floating planets, over a period of100~Myr, in star clusters without an IMBH, and in clusters with a central IMBHof mass $100~M_\odot$ or $200~M_\odot$. In the central region ($r\lesssim0.2$~pc), the IMBH's tidal influence on planetary systems is typically 10~timesstronger than the average neighbour star. For a star cluster with a$200M_\odot$ IMBH, the region in which the IMBH's influence is stronger withinthe virial radius ($\sim 1$~pc). The IMBH quenches mass segregation, and thestars in the core tend to move towards intermediate regions. The ejection rateof both stars and planets is higher when an IMBH is present. The rate at whichplanets are expelled from their host star rate is higher for clusters withhigher IMBH masses, for $t<0.5 t_{rh}$, while remains mostly constant while thestar cluster fills its Roche lobe, similar to a star cluster without an IMBH.The disruption rate of planetary systems is higher in initially denserclusters, and for wider planetary orbits, but this rate is substantiallyenhanced by the presence of a central IMBH.

Planetary Systems in a Star Cluster II: intermediate-mass black holes and planetary systems