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dc.contributor.authorLehmann, L. T.
dc.contributor.authorJardine, M. M.
dc.contributor.authorVidotto, A. A.
dc.contributor.authorMackay, D. H.
dc.contributor.authorSee, V.
dc.contributor.authorDonati, J.-F.
dc.contributor.authorFolsom, C. P.
dc.contributor.authorJeffers, S. V.
dc.contributor.authorMarsden, S. C.
dc.contributor.authorMorin, J.
dc.contributor.authorPetit, P.
dc.date.accessioned2016-11-23T11:30:16Z
dc.date.available2016-11-23T11:30:16Z
dc.date.issued2017-03-21
dc.identifier.citationLehmann , L T , Jardine , M M , Vidotto , A A , Mackay , D H , See , V , Donati , J-F , Folsom , C P , Jeffers , S V , Marsden , S C , Morin , J & Petit , P 2017 , ' The energy budget of stellar magnetic fields : comparing non-potential simulations and observations ' , Monthly Notices of the Royal Astronomical Society: Letters , vol. 466 , no. 1 , pp. L24-L28 . https://doi.org/10.1093/mnrasl/slw225en
dc.identifier.issn1745-3925
dc.identifier.otherPURE: 247676731
dc.identifier.otherPURE UUID: a1a102d2-a702-4214-afa7-e012d840e2e2
dc.identifier.otherBibCode: 2016arXiv161008314L
dc.identifier.otherScopus: 85018344806
dc.identifier.otherWOS: 000410059100006
dc.identifier.otherORCID: /0000-0001-6065-8531/work/133726084
dc.identifier.otherORCID: /0000-0002-1466-5236/work/133734288
dc.identifier.urihttps://hdl.handle.net/10023/9869
dc.descriptionLTL acknowledges support from the Scottish Universities Physics Alliance (SUPA) prize studentship and the University of St Andrews Higgs studentship. MMJ and VS acknowledge a Science & Technology Facilities Council (STFC) postdoctoral fellowship.en
dc.description.abstractThe magnetic geometry of the surface magnetic fields of more than 55 cool stars have now been mapped using spectropolarimetry. In order to better understand these observations, we compare the magnetic fieldt opology at different surface scale sizes of observed and simulated cool stars. For ease of comparison between the high-resolution non-potential magnetofrictional simulations and the relatively low-resolution observations, we filter out the small-scale field in the simulations using a spherical harmonics decomposition. We show that the large-scalefield topologies of the solar-based simulations produce values of poloidal/toroidal fields and fractions of energy in axisymmetric modes that are similar to the observations. These global non-potential evolution model simulations capture key magnetic features of the observed solar-like stars through the processes of surface flux transport and magnetic flux emergence. They do not, however, reproduce the magnetic field of M-dwarfs or stars with dominantly toroidal field.Furthermore, we analyse the magnetic field topologies of individual spherical harmonics for the simulations and discover that the dipole is predominately poloidal, while the quadrupole shows the highest fraction of toroidal fields. Magnetic field structures smaller than a quadrupole display a fixed ratio between the poloidal and toroidal magnetic energies.
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society: Lettersen
dc.rights© 2016, 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 mnrasl.oxfordjournals.org / https://doi.org/10.1093/mnrasl/slw225en
dc.subjectStars: activityen
dc.subjectStars: magnetic fielden
dc.subjectStars: solar typeen
dc.subjectMethods: analyticalen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectNDASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleThe energy budget of stellar magnetic fields : comparing non-potential simulations and observationsen
dc.typeJournal articleen
dc.contributor.sponsorScience & Technology Facilities Councilen
dc.description.versionPostprinten
dc.contributor.institutionUniversity of St Andrews. School of Physics and Astronomyen
dc.contributor.institutionUniversity of St Andrews. Applied Mathematicsen
dc.identifier.doihttps://doi.org/10.1093/mnrasl/slw225
dc.description.statusPeer revieweden
dc.identifier.urlhttp://adsabs.harvard.edu/abs/2016arXiv161008314Len
dc.identifier.grantnumberST/M001296/1en


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