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dc.contributor.authorJermyn, AS
dc.contributor.authorTout, Christopher
dc.contributor.authorChitre, SM
dc.date.accessioned2018-12-01T00:30:23Z
dc.date.available2018-12-01T00:30:23Z
dc.date.issued2018-11
dc.identifier.issn0035-8711
dc.identifier.urihttps://www.repository.cam.ac.uk/handle/1810/286187
dc.description.abstractConvection in the cores of massive stars becomes anisotropic when they rotate. This anisotropy leads to a misalignment of the thermal gradient and the thermal flux, which in turn results in baroclinicity and circulation currents in the upper radiative zone. We show that this induces a much stronger meridional flow in the radiative zone than previously thought. This drives significantly enhanced mixing, though this mixing does not necessarily reach the surface. The extra mixing takes on a similar form to convective overshooting, and is relatively insensitive to the rotation rate above a threshold, and may help explain the large overshoot distances inferred from observations. This has significant consequences for the evolution of these stars by enhancing core-envelope mixing.
dc.publisherOxford University Press (OUP)
dc.titleEnhanced rotational mixing in the radiative zones of massive stars
dc.typeArticle
prism.endingPage5446
prism.issueIdentifier4
prism.publicationDate2018
prism.publicationNameMonthly Notices of the Royal Astronomical Society
prism.startingPage5427
prism.volume480
dc.identifier.doi10.17863/CAM.33499
dcterms.dateAccepted2018-07-08
rioxxterms.versionofrecord10.1093/MNRAS/STY1831
rioxxterms.licenseref.urihttp://www.rioxx.net/licenses/all-rights-reserved
rioxxterms.licenseref.startdate2018-01-01
dc.contributor.orcidTout, Christopher [0000-0002-1556-9449]
dc.identifier.eissn1365-2966
dc.publisher.urlhttp://dx.doi.org/10.1093/mnras/sty1831
rioxxterms.typeJournal Article/Review
cam.issuedOnline2018-08-01
rioxxterms.freetoread.startdate2019-01-01


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