Collisions in primordial star clusters: formation pathway for intermediate mass black holes

Detalhes bibliográficos
Autor(a) principal: Reinoso, B.
Data de Publicação: 2018
Outros Autores: Schleicher, D. R. G., Fellhauer, M., Klessen, R. S., Boekholt, T. C. N.
Tipo de documento: Artigo
Idioma: eng
Título da fonte: Repositório Científico de Acesso Aberto de Portugal (Repositórios Cientìficos)
Texto Completo: http://hdl.handle.net/10773/25026
Resumo: Collisions were suggested to potentially play a role in the formation of massive stars in present day clusters, and have likely been relevant during the formation of massive stars and intermediate mass black holes within the first star clusters. In the early Universe, the first stellar clusters were particularly dense, as fragmentation typically only occurred at densities above $10^9$cm$^{-3}$, and the radii of the protostars were enhanced due to the larger accretion rates, suggesting a potentially more relevant role of stellar collisions. We present here a detailed parameter study to assess how the number of collisions as well as the mass growth of the most massive object depends on the properties of the cluster, and we characterize the time evolution with three effective parameters, the time when most collisions occur, the duration of the collisions period, as well as the normalization required to obtain the total number of collisions. We apply our results to typical Population III (Pop.III) clusters of about $1000$M$_\odot$, finding that a moderate enhancement of the mass of the most massive star by a factor of a few can be expected. For more massive Pop.III clusters as expected in the first atomic cooling halos, we expect a more significant enhancement by a factor of $15-32$. We therefore conclude that collisions in massive Pop.III clusters were likely relevant to form the first intermediate mass black holes.
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spelling Collisions in primordial star clusters: formation pathway for intermediate mass black holesCollisions were suggested to potentially play a role in the formation of massive stars in present day clusters, and have likely been relevant during the formation of massive stars and intermediate mass black holes within the first star clusters. In the early Universe, the first stellar clusters were particularly dense, as fragmentation typically only occurred at densities above $10^9$cm$^{-3}$, and the radii of the protostars were enhanced due to the larger accretion rates, suggesting a potentially more relevant role of stellar collisions. We present here a detailed parameter study to assess how the number of collisions as well as the mass growth of the most massive object depends on the properties of the cluster, and we characterize the time evolution with three effective parameters, the time when most collisions occur, the duration of the collisions period, as well as the normalization required to obtain the total number of collisions. We apply our results to typical Population III (Pop.III) clusters of about $1000$M$_\odot$, finding that a moderate enhancement of the mass of the most massive star by a factor of a few can be expected. For more massive Pop.III clusters as expected in the first atomic cooling halos, we expect a more significant enhancement by a factor of $15-32$. We therefore conclude that collisions in massive Pop.III clusters were likely relevant to form the first intermediate mass black holes.EDP Sciences2019-01-09T18:07:33Z2018-06-01T00:00:00Z2018-06-01info:eu-repo/semantics/publishedVersioninfo:eu-repo/semantics/articleapplication/pdfhttp://hdl.handle.net/10773/25026eng0004-636110.1051/0004-6361/201732224Reinoso, B.Schleicher, D. R. G.Fellhauer, M.Klessen, R. S.Boekholt, T. C. N.info:eu-repo/semantics/openAccessreponame:Repositório Científico de Acesso Aberto de Portugal (Repositórios Cientìficos)instname:Agência para a Sociedade do Conhecimento (UMIC) - FCT - Sociedade da Informaçãoinstacron:RCAAP2024-02-22T11:48:29Zoai:ria.ua.pt:10773/25026Portal AgregadorONGhttps://www.rcaap.pt/oai/openaireopendoar:71602024-03-20T02:58:21.201416Repositório Científico de Acesso Aberto de Portugal (Repositórios Cientìficos) - Agência para a Sociedade do Conhecimento (UMIC) - FCT - Sociedade da Informaçãofalse
dc.title.none.fl_str_mv Collisions in primordial star clusters: formation pathway for intermediate mass black holes
title Collisions in primordial star clusters: formation pathway for intermediate mass black holes
spellingShingle Collisions in primordial star clusters: formation pathway for intermediate mass black holes
Reinoso, B.
title_short Collisions in primordial star clusters: formation pathway for intermediate mass black holes
title_full Collisions in primordial star clusters: formation pathway for intermediate mass black holes
title_fullStr Collisions in primordial star clusters: formation pathway for intermediate mass black holes
title_full_unstemmed Collisions in primordial star clusters: formation pathway for intermediate mass black holes
title_sort Collisions in primordial star clusters: formation pathway for intermediate mass black holes
author Reinoso, B.
author_facet Reinoso, B.
Schleicher, D. R. G.
Fellhauer, M.
Klessen, R. S.
Boekholt, T. C. N.
author_role author
author2 Schleicher, D. R. G.
Fellhauer, M.
Klessen, R. S.
Boekholt, T. C. N.
author2_role author
author
author
author
dc.contributor.author.fl_str_mv Reinoso, B.
Schleicher, D. R. G.
Fellhauer, M.
Klessen, R. S.
Boekholt, T. C. N.
description Collisions were suggested to potentially play a role in the formation of massive stars in present day clusters, and have likely been relevant during the formation of massive stars and intermediate mass black holes within the first star clusters. In the early Universe, the first stellar clusters were particularly dense, as fragmentation typically only occurred at densities above $10^9$cm$^{-3}$, and the radii of the protostars were enhanced due to the larger accretion rates, suggesting a potentially more relevant role of stellar collisions. We present here a detailed parameter study to assess how the number of collisions as well as the mass growth of the most massive object depends on the properties of the cluster, and we characterize the time evolution with three effective parameters, the time when most collisions occur, the duration of the collisions period, as well as the normalization required to obtain the total number of collisions. We apply our results to typical Population III (Pop.III) clusters of about $1000$M$_\odot$, finding that a moderate enhancement of the mass of the most massive star by a factor of a few can be expected. For more massive Pop.III clusters as expected in the first atomic cooling halos, we expect a more significant enhancement by a factor of $15-32$. We therefore conclude that collisions in massive Pop.III clusters were likely relevant to form the first intermediate mass black holes.
publishDate 2018
dc.date.none.fl_str_mv 2018-06-01T00:00:00Z
2018-06-01
2019-01-09T18:07:33Z
dc.type.status.fl_str_mv info:eu-repo/semantics/publishedVersion
dc.type.driver.fl_str_mv info:eu-repo/semantics/article
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dc.identifier.uri.fl_str_mv http://hdl.handle.net/10773/25026
url http://hdl.handle.net/10773/25026
dc.language.iso.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv 0004-6361
10.1051/0004-6361/201732224
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dc.publisher.none.fl_str_mv EDP Sciences
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