Kavli Affiliate: Rainer Spurzem
| First 5 Authors: Francesco Flammini Dotti, M. B. N. Kouwenhoven, Qi Shu, Wei Hao, Rainer Spurzem
| Summary:
Most stars form in dense stellar environments. It is speculated that some
dense star clusters may host intermediate-mass black holes (IMBHs), which may
have formed from runaway collisions between high-mass stars, or from the
mergers of less massive black holes. Here, we numerically explore the evolution
of populations of planets in star clusters with an IMBH. We study the dynamical
evolution of single-planet systems and free-floating planets, over a period of
100~Myr, in star clusters without an IMBH, and in clusters with a central IMBH
of mass $100~M_odot$ or $200~M_odot$. In the central region ($rlesssim
0.2$~pc), the IMBH’s tidal influence on planetary systems is typically 10~times
stronger than the average neighbour star. For a star cluster with a
$200M_odot$ IMBH, the region in which the IMBH’s influence is stronger within
the virial radius ($sim 1$~pc). The IMBH quenches mass segregation, and the
stars in the core tend to move towards intermediate regions. The ejection rate
of both stars and planets is higher when an IMBH is present. The rate at which
planets are expelled from their host star rate is higher for clusters with
higher IMBH masses, for $t<0.5 t_{rh}$, while remains mostly constant while the
star cluster fills its Roche lobe, similar to a star cluster without an IMBH.
The disruption rate of planetary systems is higher in initially denser
clusters, and for wider planetary orbits, but this rate is substantially
enhanced by the presence of a central IMBH.
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