J/A+A/689/A34ivo://CDS.VizieR/J/A+A/689/A34doi:10.26093/cds/vizier.36890034CDSVergara M.C.Schleicher D.R.G.Escala A.Reinoso B.Flammini Dotti F.,Kamlah A.W.H.Liempi M.Hoyer N.Neumayer N.Spurzem R.2024-11-21T20:02:58Z2024-08-30T09:19:41ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frastronomical-modelsblack-holesquasarsstellar-associationsstellar-massesThis paper explores the theoretical relation between star clusters and black holes within, focusing on the potential role of Nuclear Star Clusters (NSCs), Globular Clusters (GCs), and Ultra Compact Dwarf Galaxies (UCDs) as environments that lead to black hole formation through stellar collisions. The study aims to identify optimal conditions for stellar collisions in different stellar systems leading to the formation of very massive stars that subsequently collapse into black holes. Data from numerical simulations and observations of diverse stellar systems are analyzed, encompassing various initial conditions, initial mass functions, and stellar evolution scenarios. We compute a critical mass, determined by the interplay of collision time, system age, and initial properties of the star cluster. The efficiency of black hole formation ({epsilon}_BH_) is defined as the ratio of initial stellar mass divided by critical mass. The study finds out that stellar systems with a ratio of initial stellar mass over critical mass above 1 exhibit high efficiencies of black hole formation, ranging from 30-100%. While there is some scatter, potentially attributed to complex system histories and the presence of gas, the results highlight the potential for achieving high efficiencies through a purely collisional channel in black hole formation. In conclusion, this theoretical exploration elucidates the connection between star clusters and black hole formation. The study underscores the significance of UCDs, GCs, and NSCs as environments conducive to stellar collisions leading to black hole formation. The defined black hole formation efficiency ({epsilon}_BH_) is shown to be influenced by the ratio of initial stellar mass to critical mass.2024A&A...689A..34Vhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/689/A34CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/689/A34https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/689/A34http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/689/A34https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/689/A34https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/689/A34http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/689/A34GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/A+A/689/A34/table1Initial conditions for simulation setsRefReference (G2)meta.ref;pos.framecharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintMiniInitial masssolMassphys.massdoubleRhHalf-Mass radiuspcphys.size.radiusfloatNNumber of starsmeta.numberintMBHBlack hole masssolMassphys.massdoubletauSimulation timeMyrtime.epochfloatCodeCode name (G1)meta.codecharJ/A+A/689/A34/table2Initial conditions for simulation sets with external potentialrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintMiniInitial masssolMassphys.massintRhHalf-Mass radiuspcphys.size.radiusfloatNNumber of starsmeta.numberintMBHBlack hole masssolMassphys.massinttauSimulation timeMyrtime.epochfloatqMass ratio between gas and starsphys.massfloatCodeCode name (G1)meta.codecharRefReference (G2)meta.ref;pos.framechar