The Origin of Massive Stars: The Inertial-inflow Model

We a dress the problem of the origin of massive stars, namely the origin, path, and timescale of the mass flows that create them. Based on extensive numerical simulations, we propose a scenario where massive stars are assembled by large-scale, converging, inertial flows that naturally occur in super...

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Detalhes bibliográficos
Autores: Padoan, Paolo, Pan, Liubin, Juvela, Mika, Haugbølle, Troels, Nordlund, Åke
Tipo de documento: artigo
Estado:Versión enviada para evaluación y publicación
Data de publicação:2020
País:España
Recursos:Consejo Superior de Investigaciones Científicas (CSIC)
Repositório:DIGITAL.CSIC. Repositorio Institucional del CSIC
OAI Identifier:oai:digital.csic.es:10261/235616
Acesso em linha:http://hdl.handle.net/10261/235616
Access Level:Acceso aberto
Palavra-chave:ISM: kinematics and dynamics
MHD
Stars: formation
Turbulence
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oai_identifier_str oai:digital.csic.es:10261/235616
network_acronym_str ES
network_name_str España
repository_id_str
dc.title.none.fl_str_mv The Origin of Massive Stars: The Inertial-inflow Model
title The Origin of Massive Stars: The Inertial-inflow Model
spellingShingle The Origin of Massive Stars: The Inertial-inflow Model
Padoan, Paolo
ISM: kinematics and dynamics
MHD
Stars: formation
Turbulence
title_short The Origin of Massive Stars: The Inertial-inflow Model
title_full The Origin of Massive Stars: The Inertial-inflow Model
title_fullStr The Origin of Massive Stars: The Inertial-inflow Model
title_full_unstemmed The Origin of Massive Stars: The Inertial-inflow Model
title_sort The Origin of Massive Stars: The Inertial-inflow Model
dc.creator.none.fl_str_mv Padoan, Paolo
Pan, Liubin
Juvela, Mika
Haugbølle, Troels
Nordlund, Åke
author Padoan, Paolo
author_facet Padoan, Paolo
Pan, Liubin
Juvela, Mika
Haugbølle, Troels
Nordlund, Åke
author_role author
author2 Pan, Liubin
Juvela, Mika
Haugbølle, Troels
Nordlund, Åke
author2_role author
author
author
author
dc.contributor.none.fl_str_mv Ministerio de Economía y Competitividad (España)
Ministerio de Ciencia, Innovación y Universidades (España)
Danish Council for Independent Research
Academy of Finland
NASA
Ames Research Center
University of Copenhagen
Villum Fonden
Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]
dc.subject.none.fl_str_mv ISM: kinematics and dynamics
MHD
Stars: formation
Turbulence
topic ISM: kinematics and dynamics
MHD
Stars: formation
Turbulence
description We a dress the problem of the origin of massive stars, namely the origin, path, and timescale of the mass flows that create them. Based on extensive numerical simulations, we propose a scenario where massive stars are assembled by large-scale, converging, inertial flows that naturally occur in supersonic turbulence. We refer to this scenario of massive-star formation as the inertial-inflow model. This model stems directly from the idea that the mass distribution of stars is primarily the result of turbulent fragmentation. Under this hypothesis, the statistical properties of turbulence determine the formation timescale and mass of prestellar cores, posing definite constraints on the formation mechanism of massive stars. We quantify such constraints by analyzing a simulation of supernova-driven turbulence in a 250 pc region of the interstellar medium, describing the formation of hundreds of massive stars over a time of approximately 30 Myr. Due to the large size of our statistical sample, we can say with full confidence that massive stars in general do not form from the collapse of massive cores nor from competitive accretion, as both models are incompatible with the numerical results. We also compute synthetic continuum observables in the Herschel and ALMA bands. We find that, depending on the distance of the observed regions, estimates of core mass based on commonly used methods may exceed the actual core masses by up to two orders of magnitude and that there is essentially no correlation between estimated and real core masses.
publishDate 2020
dc.date.none.fl_str_mv 2020
2021
2021
2021
dc.type.none.fl_str_mv info:eu-repo/semantics/article
http://purl.org/coar/resource_type/c_6501
Preprint
info:eu-repo/semantics/submittedVersion
format article
status_str submittedVersion
dc.identifier.none.fl_str_mv http://hdl.handle.net/10261/235616
url http://hdl.handle.net/10261/235616
dc.language.none.fl_str_mv Inglés
language_invalid_str_mv Inglés
dc.relation.none.fl_str_mv #PLACEHOLDER_PARENT_METADATA_VALUE#
info:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2017-2020/t AYA2017-88754-P
http://doi.org/10.3847/1538-4357/abaa47
Sí
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
eu_rights_str_mv openAccess
dc.publisher.none.fl_str_mv IOP Publishing
publisher.none.fl_str_mv IOP Publishing
dc.source.none.fl_str_mv reponame:DIGITAL.CSIC. Repositorio Institucional del CSIC
instname:Consejo Superior de Investigaciones Científicas (CSIC)
instname_str Consejo Superior de Investigaciones Científicas (CSIC)
reponame_str DIGITAL.CSIC. Repositorio Institucional del CSIC
collection DIGITAL.CSIC. Repositorio Institucional del CSIC
repository.name.fl_str_mv
repository.mail.fl_str_mv
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spelling The Origin of Massive Stars: The Inertial-inflow ModelPadoan, PaoloPan, LiubinJuvela, MikaHaugbølle, TroelsNordlund, ÅkeISM: kinematics and dynamicsMHDStars: formationTurbulenceWe a dress the problem of the origin of massive stars, namely the origin, path, and timescale of the mass flows that create them. Based on extensive numerical simulations, we propose a scenario where massive stars are assembled by large-scale, converging, inertial flows that naturally occur in supersonic turbulence. We refer to this scenario of massive-star formation as the inertial-inflow model. This model stems directly from the idea that the mass distribution of stars is primarily the result of turbulent fragmentation. Under this hypothesis, the statistical properties of turbulence determine the formation timescale and mass of prestellar cores, posing definite constraints on the formation mechanism of massive stars. We quantify such constraints by analyzing a simulation of supernova-driven turbulence in a 250 pc region of the interstellar medium, describing the formation of hundreds of massive stars over a time of approximately 30 Myr. Due to the large size of our statistical sample, we can say with full confidence that massive stars in general do not form from the collapse of massive cores nor from competitive accretion, as both models are incompatible with the numerical results. We also compute synthetic continuum observables in the Herschel and ALMA bands. We find that, depending on the distance of the observed regions, estimates of core mass based on commonly used methods may exceed the actual core masses by up to two orders of magnitude and that there is essentially no correlation between estimated and real core masses.PP acknowledges support by the Spanish MINECO under project AYA2017-88754-P. The work of ˚AN was supported by grant 1323-00199B from the Danish Council for Independent Research (DFF), and by the Centre for Star and Planet Formation, which is funded by the Danish National Research Foundation (DNRF97). LP acknowledges financial support from NSFC under grant No. 11973098. MJ acknowledges the support of the Academy of Finland Grant No. 285769. Computing resources for this work were provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center. We thankfully acknowledge the computer resources at MareNostrum and the technical support provided by Barcelona Supercomputing Center (AECT-2018-3-0019). We acknowledge PRACE for awarding us access to Curie at GENCI@CEA, France. Storage and computing resources at the University of Copenhagen HPC centre, funded in part by Villum Fonden (VKR023406), were used to carry out part of the data analysis. We thank the anonymous referee for a very useful report and the following colleagues for reading the first draft and providing comments: Philippe André, Javier Ballesteros-Paredes, Henrik Beuther, Gilles Chabrier, Lee Hartmann, Patrick Hennebelle, Alessio Traficante, Enrique Vazquez-Semadeni. Special thanks to Patricio Sanhueza and Delphine Russeil for providing the electronic tables to compute the observational core mass functions shown in Figure 26, and to Alessio Traficante for many instructive discussions on the observations of infall rates in massive clumps, and for providing the electronic tables to produce the plots in Figures 29 and 30.IOP PublishingMinisterio de Economía y Competitividad (España)Ministerio de Ciencia, Innovación y Universidades (España)Danish Council for Independent ResearchAcademy of FinlandNASAAmes Research CenterUniversity of CopenhagenVillum FondenConsejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]2021202120202021info:eu-repo/semantics/articlehttp://purl.org/coar/resource_type/c_6501Preprintinfo:eu-repo/semantics/submittedVersionhttp://hdl.handle.net/10261/235616reponame:DIGITAL.CSIC. Repositorio Institucional del CSICinstname:Consejo Superior de Investigaciones Científicas (CSIC)Inglés#PLACEHOLDER_PARENT_METADATA_VALUE#info:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2017-2020/t AYA2017-88754-Phttp://doi.org/10.3847/1538-4357/abaa47Síinfo:eu-repo/semantics/openAccessoai:digital.csic.es:10261/2356162026-05-22T06:33:51Z
score 15,812429

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