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dc.contributor.authorLehmann, L. T.
dc.contributor.authorJardine, M. M.
dc.contributor.authorMackay, D. H.
dc.contributor.authorVidotto, A. A.
dc.identifier.citationLehmann , L T , Jardine , M M , Mackay , D H & Vidotto , A A 2018 , ' Connecting the large- and the small-scale magnetic fields of solar-like stars ' , Monthly Notices of the Royal Astronomical Society , vol. 478 , no. 4 , pp. 4390-4409 .
dc.identifier.otherPURE: 255426340
dc.identifier.otherPURE UUID: 6854e267-6477-4ba8-9f9b-2cda664a7eb7
dc.identifier.otherScopus: 85050812430
dc.identifier.otherORCID: /0000-0001-6065-8531/work/58055429
dc.identifier.otherWOS: 000441288300009
dc.identifier.otherORCID: /0000-0002-1466-5236/work/57821828
dc.descriptionLTL acknowledges support from the Scottish Universities Physics Alliance (SUPA) prize studentship and the University of St Andrews Higgs studentship. MMJ acknowledges the support of the Science & Technology Facilities Council (STFC) (ST/M001296/1).en
dc.description.abstractA key question in understanding the observed magnetic field topologies of cool stars is the link between the small- and the large-scalemagnetic field and the influence of the stellar parameters on the magnetic field topology. We examine various simulated stars to connect the small scale with the observable large-scale field. The highly resolved 3D simulations we used couple a flux transport model with a non-potential coronal model using a magnetofrictional technique. The surface magnetic field of these simulations is decomposed into spherical harmonics which enables us to analyse the magnetic field topologies on a wide range of length scales and to filter the large-scale magnetic field for a direct comparison with the observations. We show that the large-scale field of the self-consistent simulations fits the observed solar-like stars and is mainly set up by the global dipolar field and the large-scale properties of the flux pattern, e.g. the averaged latitudinal position of the emerging small-scale field and its global polarity pattern. The stellar parameter flux emergence rate, differential rotation, and meridional flow affect the large-scale magnetic field topology. An increased flux emergence rate increases the magnetic flux in all field components and an increased differential rotation increases the toroidal field fraction by decreasing the poloidal field. The meridional flow affects the distribution of the magnetic energy across the spherical harmonic modes.
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 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:
dc.subjectMethods: analyticalen
dc.subjectStars: activityen
dc.subjectStars: magnetic fielden
dc.subjectStars: solar-typeen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectAstronomy and Astrophysicsen
dc.subjectSpace and Planetary Scienceen
dc.titleConnecting the large- and the small-scale magnetic fields of solar-like starsen
dc.typeJournal articleen
dc.contributor.institutionUniversity of St Andrews.School of Physics and Astronomyen
dc.contributor.institutionUniversity of St Andrews.Applied Mathematicsen
dc.description.statusPeer revieweden

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