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SUMMARY:The formation of intermediate-mass and upper mass gap black holes 
 in dense star clusters with up to 1 million stars - Manuel Arca Sedda
DTSTART:20230605T130000Z
DTEND:20230605T140000Z
UID:TALK201301@talks.cam.ac.uk
CONTACT:Alexander Rasskazov
DESCRIPTION:The processes that govern the formation of intermediate-mass b
 lack holes (IMBHs)\nin dense stellar clusters are still unclear. In this t
 alk I will discuss the role of stellar mergers\, star-BH interactions and 
 accretion\, as well as BH binary (BBH) mergers in seeding and growing IMBH
 s in the Dragon-II simulation database\, a suite of 19 direct N-body model
 s representing dense clusters with up to 10^6 stars. We will discuss mass 
 and spin of IMBHs in Dragon-II simulations\, showing that there is a link 
 between the route to IMBH formation and the host cluster structure. In clu
 sters denser than 3 × 10^5 Msun pc^-3\, the collapse of massive star coll
 ision products represents the dominant IMBH formation process\, leading to
  the formation of heavy IMBHs (mIMBH > 200 Msun )\, possibly slowly rotati
 ng\, that form over times < 5 Myr and grow further via stellar accretion a
 nd mergers in just < 30 Myr. BBH mergers are the dominant IMBH formation c
 hannel in less dense clusters\, for which we find that the looser the clus
 ter\, the longer the formation time (10 − 300 Myr) and the larger the IM
 BH mass\, although remaining within 200 Msun. Strong dynamical scatterings
  and relativistic recoil efficiently eject all IMBHs in Dragon-II clusters
 \, suggesting that IMBHs in this type of clusters are unlikely to grow bey
 ond a few 10^2 Msun.
LOCATION:Streaming online and in MR14
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