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dc.contributor.authorKrause, Martin G. H.
dc.contributor.authorOffner, Stella S. R.
dc.contributor.authorCharbonnel, Corinne
dc.contributor.authorGieles, Mark
dc.contributor.authorKlessen, Ralf S.
dc.contributor.authorVazquez-Semadeni, Enrique
dc.contributor.authorBallesteros-Paredes, Javier
dc.contributor.authorGirichidis, Philipp
dc.contributor.authorKruijssen, J. M. Diederik
dc.contributor.authorWard, Jacob L.
dc.contributor.authorZinnecker, Hans
dc.date.accessioned2020-10-09T00:09:24Z
dc.date.available2020-10-09T00:09:24Z
dc.date.issued2020-06-02
dc.identifier.citationKrause , M G H , Offner , S S R , Charbonnel , C , Gieles , M , Klessen , R S , Vazquez-Semadeni , E , Ballesteros-Paredes , J , Girichidis , P , Kruijssen , J M D , Ward , J L & Zinnecker , H 2020 , ' The Physics of Star Cluster Formation and Evolution ' , Space Science Reviews , vol. 216 , 64 . https://doi.org/10.1007/s11214-020-00689-4
dc.identifier.issn0038-6308
dc.identifier.otherPURE: 21238090
dc.identifier.otherPURE UUID: e46ed760-d942-4431-abad-5d728582b94f
dc.identifier.otherArXiv: http://arxiv.org/abs/2005.00801v1
dc.identifier.otherORCID: /0000-0002-9610-5629/work/81741733
dc.identifier.otherScopus: 85083956766
dc.identifier.urihttp://hdl.handle.net/2299/23221
dc.description© 2020 Springer-Verlag. The final publication is available at Springer via https://doi.org/10.1007/s11214-020-00689-4.
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 effectively 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.en
dc.format.extent46
dc.language.isoeng
dc.relation.ispartofSpace Science Reviews
dc.subjectastro-ph.GA
dc.subjectastro-ph.SR
dc.titleThe Physics of Star Cluster Formation and Evolutionen
dc.contributor.institutionCentre for Astrophysics Research
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.description.statusPeer reviewed
dc.date.embargoedUntil2021-06-02
rioxxterms.versionAM
rioxxterms.versionofrecordhttps://doi.org/10.1007/s11214-020-00689-4
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue


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