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Protostellar feedback in turbulent fragmentation: consequences for stellar clustering and multiplicity

Guszejnov, David; Hopkins, Philip F.; Krumholz, Mark

Description

Stars are strongly clustered on both large (∼pc) and small (∼binary) scales, but there are few analytic or even semi-analytic theories for the correlation function and multiplicity of stars. In this paper, we present such a theory, based on our recently developed semi-analytic framework called MISFIT (Minimalistic Star Formation Including Turbulence), which models gravitoturbulent fragmentation, including the suppression of fragmentation by protostellar radiation feedback. We compare the...[Show more]

dc.contributor.authorGuszejnov, David
dc.contributor.authorHopkins, Philip F.
dc.contributor.authorKrumholz, Mark
dc.date.accessioned2021-09-06T04:21:29Z
dc.date.available2021-09-06T04:21:29Z
dc.identifier.issn0035-8711
dc.identifier.urihttp://hdl.handle.net/1885/247377
dc.description.abstractStars are strongly clustered on both large (∼pc) and small (∼binary) scales, but there are few analytic or even semi-analytic theories for the correlation function and multiplicity of stars. In this paper, we present such a theory, based on our recently developed semi-analytic framework called MISFIT (Minimalistic Star Formation Including Turbulence), which models gravitoturbulent fragmentation, including the suppression of fragmentation by protostellar radiation feedback. We compare the results including feedback to a control model in which it is omitted. We show that both classes of models robustly reproduce the stellar correlation function at >0.01 pc scales, which is well approximated by a power law that follows generally from scale-free physics (turbulence plus gravity) on large scales. On smaller scales, protostellar disc fragmentation becomes dominant over common core fragmentation, leading to a steepening of the correlation function. Multiplicity is more sensitive to feedback: we found that a model with the protostellar heating reproduces the observed multiplicity fractions and mass ratio distributions for both Solar and sub-Solar mass stars (in particular, the brown dwarf desert), while a model without feedback fails to do so. The model with feedback also produces an at-formation period distribution consistent with the one inferred from observations. However, it is unable to produce short-range binaries below the length-scale of protostellar discs. We suggest that such close binaries are produced primarily by disc fragmentation and further decrease their separation through orbital decay.
dc.format.mimetypeapplication/pdf
dc.language.isoen_AU
dc.publisherOxford University Press (OUP)
dc.rights© 2017 The Authors
dc.sourceMonthly Notices of the Royal Astronomical Society
dc.subjectturbulence
dc.subjectbinaries: general
dc.subjectstars: formation
dc.subjectgalaxies: star clusters: general
dc.subjectgalaxies: star formation
dc.subjectcosmology: theory
dc.titleProtostellar feedback in turbulent fragmentation: consequences for stellar clustering and multiplicity
dc.typeJournal article
local.description.notesImported from ARIES
local.identifier.citationvolume468
dc.date.issued2017
local.identifier.absfor020110 - Stellar Astronomy and Planetary Systems
local.identifier.ariespublicationu5058514xPUB95
local.publisher.urlhttp://www.oxfordjournals.org/
local.type.statusPublished Version
local.contributor.affiliationGuszejnov, David, California Institute of Technology
local.contributor.affiliationHopkins, Philip F., California Institute of Technology
local.contributor.affiliationKrumholz, Mark, College of Science, ANU
local.bibliographicCitation.issue4
local.identifier.doi10.1093/mnras/stx725
dc.date.updated2020-11-23T10:59:30Z
local.identifier.thomsonID000402819700027
dcterms.accessRightsOpen Access
dc.provenancehttps://v2.sherpa.ac.uk/id/publication/24618..."published version can be made open access in institutional repository" from SHERPA/RoMEO site (as at 6/09/21).
CollectionsANU Research Publications

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