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dc.contributor.authorWurster, J.
dc.contributor.authorBate, Matthew R.
dc.contributor.authorPrice, Daniel J.
dc.date.accessioned2019-10-25T10:30:03Z
dc.date.available2019-10-25T10:30:03Z
dc.date.issued2018-12
dc.identifier.citationWurster , J , Bate , M R & Price , D J 2018 , ' On the origin of magnetic fields in stars ' , Monthly Notices of the Royal Astronomical Society , vol. 481 , no. 2 , pp. 2450-2457 . https://doi.org/10.1093/mnras/sty2438en
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 262150209
dc.identifier.otherPURE UUID: 1c11db27-88a2-47a5-bc3c-db7aba26d03d
dc.identifier.otherBibtex: WursterBatePrice2018ff
dc.identifier.otherScopus: 85060875725
dc.identifier.otherORCID: /0000-0003-0688-5332/work/63716936
dc.identifier.urihttps://hdl.handle.net/10023/18768
dc.description.abstractAre the kG-strength magnetic fields observed in young stars a fossil field left over from their formation or are they generated by a dynamo? We use radiation non-ideal magnetohydrodynamics simulations of the gravitational collapse of a rotating, magnetized molecular cloud core over 17 orders of magnitude in density, past the first hydrostatic core to the formation of the second, stellar core, to examine the fossil field hypothesis. Whereas in previous work, we found that magnetic fields in excess of 10 kG can be implanted in stars at birth, this assumed ideal magnetohydrodynamics (MHD), i.e. that the gas is coupled to the magnetic field. Here we present non-ideal MHD calculations which include Ohmic resistivity, ambipolar diffusion, and the Hall effect. For realistic cosmic ray ionization rates, we find that magnetic field strengths of ≲ kG are implanted in the stellar core at birth, ruling out a strong fossil field. While these results remain sensitive to resolution, they cautiously provide evidence against a fossil field origin for stellar magnetic fields, suggesting instead that magnetic fields in stars originate in a dynamo process.
dc.format.extent8
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Societyen
dc.rights© 2018 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society. This work has been made available online in accordance with publisher policies or with permission. Permission for further reuse of this content should be sought from the publisher or the rights holder. This is the final published version of the work, which was originally published at https://doi.org/10.1093/mnras/sty2438en
dc.subjectMagnetic fieldsen
dc.subjectMHDen
dc.subjectMethods: numericalen
dc.subjectStars: formationen
dc.subjectQA75 Electronic computers. Computer scienceen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectDASen
dc.subject.lccQA75en
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleOn the origin of magnetic fields in starsen
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/sty2438
dc.description.statusPeer revieweden
dc.identifier.urlhttps://arxiv.org/abs/1809.01234en


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