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dc.contributor.authorDavies, Claire
dc.contributor.authorGregory, Scott
dc.contributor.authorGreaves, Jane Sophia
dc.date.accessioned2014-12-08T15:01:05Z
dc.date.available2014-12-08T15:01:05Z
dc.date.issued2014-10-21
dc.identifier.citationDavies , C , Gregory , S & Greaves , J S 2014 , ' Accretion discs as regulators of stellar angular momentum evolution in the ONC and Taurus-Auriga ' Monthly Notices of the Royal Astronomical Society , vol. 444 , no. 2 , pp. 1157-1176 . https://doi.org/10.1093/mnras/stu1488en
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 157833509
dc.identifier.otherPURE UUID: 1741029c-3da4-40fa-a1cb-d286775b066e
dc.identifier.otherWOS: 000342926300013
dc.identifier.otherScopus: 84929439142
dc.identifier.urihttp://hdl.handle.net/10023/5890
dc.descriptionCLD's PhD is supported by a Science and Technology Facilities Council (STFC) studentship from the government of UK. SGG acknowledges support from the STFC via an Ernest Rutherford Fellowship [ST/J003255/1].en
dc.description.abstractIn light of recent substantial updates to spectral type estimations and newly established intrinsic colours, effective temperatures, and bolometric corrections for pre-main sequence (PMS) stars, we re-address the theory of accretion disc-regulated stellar angular momentum (AM) evolution. We report on the compilation of a consistent sample of fully convective stars within two of the most well-studied and youngest, nearby regions of star formation: the Orion nebula Cluster and Taurus-Auriga. We calculate the average specific stellar AM (j⋆) assuming solid body rotation, using surface rotation periods gathered from the literature and new estimates of stellar radii and ages. We use published Spitzer IRAC fluxes to classify our stars as Class II or Class III and compare their j⋆ evolution. Our results suggest that disc dispersal is a rapid process that occurs at a variety of ages. We find a consistent j⋆ reduction rate between the Class II and Class III PMS stars which we interpret as indicating a period of accretion disc-regulated AM evolution followed by near-constant AM evolution once the disc has dissipated. Furthermore, assuming our observed spread in stellar ages is real, we find that the removal rate of j⋆ during the Class II phase is more rapid than expected by contraction at constant stellar rotation rate. A much more efficient process of AM removal must exist, most likely in the form of an accretion-driven stellar wind or other outflow from the star-disc interaction region or extended disc surface.
dc.format.extent20
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Societyen
dc.rightsThis article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2014 The Authors, Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.en
dc.subjectAccretion, accretion discsen
dc.subjectStars: formationen
dc.subjectStars: late-typeen
dc.subjectStars: pre-main-sequenceen
dc.subjectStars: rotationen
dc.subjectStars: variables: T Tauri, Herbig Ae/Been
dc.subjectPre-main sequenceen
dc.subjectOrion-nebula-clusteren
dc.subjectLow-mass starsen
dc.subjectVery-low massen
dc.subjectObserved luminosity spreaden
dc.subjectColor-magnitude diagramsen
dc.subjectFully convective staren
dc.subjectSolar-type starsen
dc.subjectX-ray-emissionen
dc.subjectT-Taurien
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleAccretion discs as regulators of stellar angular momentum evolution in the ONC and Taurus-Aurigaen
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews.School of Physics and Astronomyen
dc.identifier.doihttps://doi.org/10.1093/mnras/stu1488
dc.description.statusPeer revieweden
dc.identifier.urlhttp://mnras.oxfordjournals.org/content/444/2/1157.full#sec-22


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