Please use this identifier to cite or link to this item: http://hdl.handle.net/10261/237547
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dc.contributor.authorKrause, Martin G. H.es_ES
dc.contributor.authorOffner, Stella S.R.es_ES
dc.contributor.authorCharbonnel, Corinnees_ES
dc.contributor.authorGieles, Markes_ES
dc.contributor.authorKlessen, Ralf S.es_ES
dc.contributor.authorVázquez-Semadeni, Enriquees_ES
dc.contributor.authorBallesteros-Paredes, Javieres_ES
dc.contributor.authorGirichidis, Philippes_ES
dc.contributor.authorDiederik Kruijssen, J. M.es_ES
dc.contributor.authorWard, Jacob L.es_ES
dc.contributor.authorZinnecker, Hanses_ES
dc.date.accessioned2021-04-10T10:54:23Z-
dc.date.available2021-04-10T10:54:23Z-
dc.date.issued2020-
dc.identifier.citationSpace Science Reviews 216: 64 (2020)es_ES
dc.identifier.urihttp://hdl.handle.net/10261/237547-
dc.descriptionarXiv:2005.00801v2es_ES
dc.description.abstractStar clusters form in dense, hierarchically collapsing gas clouds. Bulk kinetic energy is transformed to turbulence with stars forming from cores fed by filaments. In the most compact regions, stellar feedback is least effective in removing the gas and stars may form very efficiently. These are also the regions where, in high-mass clusters, ejecta from some kind of high-mass stars are effectively captured during the formation phase of some of the low mass stars and channeled into the latter to form multiple populations. Star formation epochs in star clusters are generally set by gas flows that determine the abundance of gas in the cluster. We argue that there is likely only one star formation epoch after which clusters remain essentially clear of gas by cluster winds. Collisional dynamics is important in this phase leading to core collapse, expansion and eventual dispersion of every cluster. We review recent developments in the field with a focus on theoretical work.es_ES
dc.description.sponsorshipJ.M.D.K. gratefully acknowledges funding from the German Research Foundation (DFG) in the form of an Emmy Noether Research Group (grant number KR4801/1-1) and a DFG Sachbeihilfe Grant (grant number KR4801/2-1), from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme via the ERC Starting Grant MUSTANG (grant agreement number 714907), and from Sonderforschungsbereich SFB 881 “The Milky Way System” (subproject B2) of the DFG. S.S.R.O. acknowledges funding from NSF Career grant AST-1650486. P.G. acknowledges funding from the European Research Council under ERC-CoG grant CRAGSMAN-646955. R.S.K. acknowledges support from the Deutsche Forschungsgemeinschaft via the SFB 881 “The Milky Way System” (subprojects B1, B2, and B8) as well as funding from the Heidelberg Cluster of Excellence STRUCTURES in the framework of Germany’s Excellence Strategy (grant EXC-2181/1-390900948). JBP acknowledges UNAM-DGAPA-PAPIIT support through grant number IN-111-219. MG acknowledges support from the ERC (CLUSTERS, StG-335936). E.V.-S. acknowledges financial support from CONACYT grant 255295.es_ES
dc.language.isoenges_ES
dc.publisherSpringer Naturees_ES
dc.relationinfo:eu-repo/grantAgreement/EC/H2020/714907es_ES
dc.relationinfo:eu-repo/grantAgreement/EC/H2020/646955es_ES
dc.relationinfo:eu-repo/grantAgreement/EC/FP7/335936es_ES
dc.rightsopenAccessen_EN
dc.titleThe physics of star cluster formation and evolutiones_ES
dc.typeartículoes_ES
dc.identifier.doi10.1007/s11214-020-00689-4-
dc.description.peerreviewedPeer reviewedes_ES
dc.relation.publisherversionhttps://doi.org/10.1007/s11214-020-00689-4es_ES
dc.identifier.e-issn1572-9672-
dc.embargo.terms2021-06-02es_ES
dc.contributor.funderGerman Research Foundationes_ES
dc.contributor.funderEuropean Research Counciles_ES
dc.contributor.funderEuropean Commissiones_ES
dc.contributor.funderComisión Nacional de Investigación Científica y Tecnológica (Chile)es_ES
dc.contributor.funderNational Science Foundation (US)es_ES
dc.relation.csices_ES
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dc.identifier.funderhttp://dx.doi.org/10.13039/501100001659es_ES
dc.identifier.funderhttp://dx.doi.org/10.13039/501100002848es_ES
dc.identifier.funderhttp://dx.doi.org/10.13039/501100000780es_ES
dc.identifier.funderhttp://dx.doi.org/10.13039/501100000781es_ES
dc.identifier.funderhttp://dx.doi.org/10.13039/100000001es_ES
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item.cerifentitytypePublications-
item.languageiso639-1en-
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