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dc.contributor.authorSmilgys, Romas
dc.contributor.authorBonnell, Ian Alexander
dc.date.accessioned2017-10-24T08:30:10Z
dc.date.available2017-10-24T08:30:10Z
dc.date.issued2017-12-21
dc.identifier.citationSmilgys , R & Bonnell , I A 2017 , ' Formation of stellar clusters ' Monthly Notices of the Royal Astronomical Society , vol. 472 , no. 4 , pp. 4982-4991 . https://doi.org/10.1093/mnras/stx2396en
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 251424791
dc.identifier.otherPURE UUID: d2f9bf49-97c0-42fd-b207-51826174dfbf
dc.identifier.otherScopus: 85052300713
dc.identifier.urihttp://hdl.handle.net/10023/11908
dc.description.abstractWe investigate the triggering of star formation and the formation of stellar clusters in molecular clouds that form as the ISM passes through spiral shocks. The spiral shock compresses gas into 100 pc long main star formation ridge, where clusters forming every 5-10pc along the merger ridge. We use a gravitational potential based cluster finding algorithm, which extracts individual clusters, calculates their physical properties and traces cluster evolution over multiple time steps. Final cluster masses at the end of simulation range between 1000 and 30000 M⊙ with their characteristic half-mass radii between 0.1 pc and 2 pc. These clusters form by gathering material from 10-20 pc size scales. Clusters also show a mass -specific angular momentum relation, where more massive clusters have larger specific angular momentum due to the larger size scales, and hence angular momentum from which they gather their mass. The evolution shows that more massive clusters experiences hierarchical merging process, which increases stellar age spreads up to 2-3 Myr. Less massive clusters appear to grow by gathering nearby recently formed sinks, while more massive clusters with their large global gravitational potentials are increasing their mass growth from gas accretion.en
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Societyen
dc.rights© 2017, the Author(s). This work has been made available online in accordance with the publisher’s policies. This is the author created, accepted version manuscript following peer review and may differ slightly from the final published version. The final published version of this work is available at https://doi.org/10.1093/mnras/stx2396en
dc.subjectStars: formationen
dc.subjectStars: luminosity function, mass functionen
dc.subjectOpen clusters and associations: generalen
dc.subjectGalaxies: star formationen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectNDASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleFormation of stellar clustersen
dc.typeJournal articleen
dc.description.versionPostprinten
dc.contributor.institutionUniversity of St Andrews. School of Physics and Astronomyen
dc.identifier.doihttps://doi.org/10.1093/mnras/stx2396
dc.description.statusPeer revieweden


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