Black Holes in Massive Star Clusters

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dc.creatorMcMillan, Steve
dc.creatorBaumgardt, Holger
dc.creatorZwart, Simon Portegies
dc.creatorHut, Piet
dc.creatorMakino, Junichiro
dc.date2004-11-06
dc.date.accessioned2026-07-07T02:15:41Z
dc.date.available2026-07-07T02:15:41Z
dc.descriptionClose encounters and physical collisions between stars in young dense clusters can result in new channels for stellar evolution, and may lead to the formation of very massive stars and black holes via runaway merging. We present some details of this process, using the results of N-body simulations and simple analytical estimates to place limits on the cluster parameters for which it expected to occur. For small clusters, the mass of the runaway is effectively limited by the total number of high-mass stars in the system. For larger clusters, the runaway mass is determined by the fraction of stars that can mass-segregate to the cluster core while still on the main sequence. In typical cases, the result is in the range commonly cited for intermediate-mass black holes. This mechanism may therefore have important implications for the formation of massive black holes and black-hole binaries in dense cluster cores.
dc.description8 pages, 2 figures; to appear in "Formation and Evolution of Massive Young Star Clusters," eds. H.J.G.L.M. Lamers, A. Nota & L.J. Smith
dc.identifierhttps://arxiv.org/abs/astro-ph/0411166
dc.identifierhttp://arxiv.org/abs/astro-ph/0411166
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/8498
dc.subjectAstrophysics
dc.titleBlack Holes in Massive Star Clusters
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