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dc.contributor.authorYeates, A. R.
dc.contributor.authorAmari, Tahar
dc.contributor.authorContopoulos, Ioannis
dc.contributor.authorFeng, Xueshang
dc.contributor.authorMackay, D. H.
dc.contributor.authorMikić, Zoran
dc.contributor.authorWiegelmann, Thomas
dc.contributor.authorHutton, Joseph
dc.contributor.authorLowder, Christopher A.
dc.contributor.authorMorgan, Huw
dc.contributor.authorPetrie, Gordon
dc.contributor.authorRachmeler, L. A.
dc.contributor.authorUpton, Lisa A.
dc.contributor.authorCanou, Aurelien
dc.contributor.authorChopin, Pierre
dc.contributor.authorDowns, Cooper
dc.contributor.authorDruckmüller, Miloslav
dc.contributor.authorLinker, Jon A.
dc.contributor.authorSeaton, Daniel B.
dc.contributor.authorTörök, Tibor
dc.identifier.citationYeates , A R , Amari , T , Contopoulos , I , Feng , X , Mackay , D H , Mikić , Z , Wiegelmann , T , Hutton , J , Lowder , C A , Morgan , H , Petrie , G , Rachmeler , L A , Upton , L A , Canou , A , Chopin , P , Downs , C , Druckmüller , M , Linker , J A , Seaton , D B & Török , T 2018 , ' Global non-potential magnetic models of the solar corona during the March 2015 eclipse ' , Space Science Reviews , vol. 214 , no. 5 , 99 .
dc.identifier.otherPURE: 255271262
dc.identifier.otherPURE UUID: c7326d4d-a769-46b4-87fc-7f54d1cb3c2c
dc.identifier.otherScopus: 85051104176
dc.identifier.otherORCID: /0000-0001-6065-8531/work/58055418
dc.identifier.otherWOS: 000441227600001
dc.descriptionFunding: UK Science and Technology Facilities Council (STFC) (ARY, DHM).en
dc.description.abstractSeven different models are applied to the same problem of simulating the Sun’s coronal magnetic field during the solar eclipse on 2015 March 20. All of the models are non-potential, allowing for free magnetic energy, but the associated electric currents are developed in significantly different ways. This is not a direct comparison of the coronal modelling techniques, in that the different models also use different photospheric boundary conditions, reflecting the range of approaches currently used in the community. Despite the significant differences, the results show broad agreement in the overall magnetic topology. Among those models with significant volume currents in much of the corona, there is general agreement that the ratio of total to potential magnetic energy should be approximately 1.4. However, there are significant differences in the electric current distributions; while static extrapolations are best able to reproduce active regions, they are unable to recover sheared magnetic fields in filament channels using currently available vector magnetogram data. By contrast, time-evolving simulations can recover the filament channel fields at the expense of not matching the observed vector magnetic fields within active regions. We suggest that, at present, the best approach may be a hybrid model using static extrapolations but with additional energization informed by simplified evolution models. This is demonstrated by one of the models.
dc.relation.ispartofSpace Science Reviewsen
dc.rights© The Author(s) 2018. This article is distributed under the terms of the Creative Commons Attribution 4.0 International License (, which permits unrestricted use, distribution, and reproduction in any medium, provided you give appropriate credit to the original author(s) and the source, provide a link to the Creative Commons license, and indicate if changes were made.en
dc.subjectMagnetic fieldsen
dc.subjectSun: surface magnetismen
dc.subjectSun: coronaen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.titleGlobal non-potential magnetic models of the solar corona during the March 2015 eclipseen
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews.Applied Mathematicsen
dc.description.statusPeer revieweden

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