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dc.contributor.authorWeinzierl, Marion
dc.contributor.authorYeates, Anthony
dc.contributor.authorMackay, Duncan Hendry
dc.contributor.authorHenney, Carl
dc.contributor.authorArge, C. Nick
dc.date.accessioned2016-06-24T09:30:04Z
dc.date.available2016-06-24T09:30:04Z
dc.date.issued2016-05-23
dc.identifier.citationWeinzierl , M , Yeates , A , Mackay , D H , Henney , C & Arge , C N 2016 , ' A new technique for the photospheric driving of non-potential solar coronal magnetic field simulations ' , Astrophysical Journal , vol. 823 , no. 1 , 55 . https://doi.org/10.3847/0004-637X/823/1/55en
dc.identifier.issn0004-637X
dc.identifier.otherPURE: 241821254
dc.identifier.otherPURE UUID: 9fbb420c-559e-4400-a889-70baf4a84175
dc.identifier.otherScopus: 84971646918
dc.identifier.otherORCID: /0000-0001-6065-8531/work/58055462
dc.identifier.otherWOS: 000377216300055
dc.identifier.urihttps://hdl.handle.net/10023/9043
dc.description.abstractIn this paper, we develop a new technique for driving global non-potential simulations of the Sun's coronal magnetic field solely from sequences of radial magnetic maps of the solar photosphere. A primary challenge to driving such global simulations is that the required horizontal electric field cannot be uniquely determined from such maps. We show that an "inductive" electric field solution similar to that used by previous authors successfully reproduces specific features of the coronal field evolution in both single and multiple bipole simulations. For these cases, the true solution is known because the electric field was generated from a surface flux-transport model. The match for these cases is further improved by including the non-inductive electric field contribution from surface differential rotation. Then, using this reconstruction method for the electric field, we show that a coronal non-potential simulation can be successfully driven from a sequence of ADAPT maps of the photospheric radial field, without including additional physical observations which are not routinely available.
dc.format.extent16
dc.language.isoeng
dc.relation.ispartofAstrophysical Journalen
dc.rights© 2016, The American Astronomical Society. This work is made available online in accordance with the publisher’s policies. This is the final published version of the work, which was originally published at iopscience.iop.org / https://dx.doi.org/10.3847/0004-637X/823/1/55en
dc.subjectMagnetohydrodynamics (MHDs)en
dc.subjectSun: coronaen
dc.subjectSun: coronal mass ejections (CMEs)en
dc.subjectSun: magnetic fieldsen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectNDASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleA new technique for the photospheric driving of non-potential solar coronal magnetic field simulationsen
dc.typeJournal articleen
dc.contributor.sponsorThe Leverhulme Trusten
dc.contributor.sponsorScience & Technology Facilities Councilen
dc.contributor.sponsorScience & Technology Facilities Councilen
dc.contributor.sponsorArts and Humanities Research Councilen
dc.contributor.sponsorScience & Technology Facilities Councilen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews. Applied Mathematicsen
dc.identifier.doihttps://doi.org/10.3847/0004-637X/823/1/55
dc.description.statusPeer revieweden
dc.identifier.grantnumberRPG-305en
dc.identifier.grantnumberPO: 4070103637en
dc.identifier.grantnumberST/K000950/1en
dc.identifier.grantnumberAH/F018398/1en
dc.identifier.grantnumberST/N000609/1en


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