%0 Generic %1 kritos2022massive %A Kritos, Konstantinos %A Berti, Emanuele %A Silk, Joseph %D 2022 %K BH Massive clusters star %T Massive black hole assembly in nuclear star clusters %U http://arxiv.org/abs/2212.06845 %X Nuclear star clusters, that fragment into metal-poor stars in situ at the centers of protogalaxies, provide ideal environments for the formation of intermediate-mass black holes with masses $10^3-10^6M_ødot$. We utilize the semi-analytic model implemented in Rapster, a public rapid cluster evolution code. We implement simple recipes for stellar collisions and gas accretion/expulsion into the code and identify the regimes where each channel contributes to the dynamical formation of intermediate-mass black holes via repeated mergers of stellar black-hole seeds. We find that intermediate-mass black hole formation is almost inevitable if the initial mean density of the nuclear cluster is $>10^8M_pc^-3$. Million solar mass black holes can form within 100 Myr in the heaviest ($>10^7M_ødot$) and most compact ($<0.5~pc$) nuclear clusters. We demonstrate that by today these resemble the observed range of nuclear clusters in dwarf galaxies and that there are potential gravitational-wave signatures of the massive black-hole formation process.

@misc{kritos2022massive, abstract = {Nuclear star clusters, that fragment into metal-poor stars in situ at the centers of protogalaxies, provide ideal environments for the formation of intermediate-mass black holes with masses $10^3-10^6M_\odot$. We utilize the semi-analytic model implemented in Rapster, a public rapid cluster evolution code. We implement simple recipes for stellar collisions and gas accretion/expulsion into the code and identify the regimes where each channel contributes to the dynamical formation of intermediate-mass black holes via repeated mergers of stellar black-hole seeds. We find that intermediate-mass black hole formation is almost inevitable if the initial mean density of the nuclear cluster is $>10^8M_\odot{\rm pc}^{-3}$. Million solar mass black holes can form within 100 Myr in the heaviest ($>10^7M_\odot$) and most compact ($<0.5~{\rm pc}$) nuclear clusters. We demonstrate that by today these resemble the observed range of nuclear clusters in dwarf galaxies and that there are potential gravitational-wave signatures of the massive black-hole formation process.}, added-at = {2022-12-15T22:54:00.000+0100}, author = {Kritos, Konstantinos and Berti, Emanuele and Silk, Joseph}, biburl = {https://www.bibsonomy.org/bibtex/2c99d5b17e0806d6d4f892fc618d0c8df/quark75}, description = {Massive black hole assembly in nuclear star clusters}, interhash = {897fcb88e6cb0a21e887765faa37d0ad}, intrahash = {c99d5b17e0806d6d4f892fc618d0c8df}, keywords = {BH Massive clusters star}, note = {cite arxiv:2212.06845Comment: 13 pages, 7 figures}, timestamp = {2022-12-15T22:54:00.000+0100}, title = {Massive black hole assembly in nuclear star clusters}, url = {http://arxiv.org/abs/2212.06845}, year = 2022 }