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dc.contributor.authorMikić, Zoran
dc.contributor.authorDowns, Cooper
dc.contributor.authorLinker, Jon A.
dc.contributor.authorCaplan, Ronald M.
dc.contributor.authorMackay, Duncan H.
dc.contributor.authorUpton, Lisa A.
dc.contributor.authorRiley, Pete
dc.contributor.authorLionello, Roberto
dc.contributor.authorTörök, Tibor
dc.contributor.authorTitov, Viacheslav S.
dc.contributor.authorWijaya, Janvier
dc.contributor.authorDruckmüller, Miloslav
dc.contributor.authorPasachoff, Jay M.
dc.contributor.authorCarlos, Wendy
dc.date.accessioned2019-03-01T00:38:15Z
dc.date.available2019-03-01T00:38:15Z
dc.date.issued2018-08-27
dc.identifier.citationMikić , Z , Downs , C , Linker , J A , Caplan , R M , Mackay , D H , Upton , L A , Riley , P , Lionello , R , Török , T , Titov , V S , Wijaya , J , Druckmüller , M , Pasachoff , J M & Carlos , W 2018 , ' Predicting the corona for the 21 August 2017 total solar eclipse ' , Nature Astronomy . https://doi.org/10.1038/s41550-018-0562-5en
dc.identifier.issn2397-3366
dc.identifier.otherPURE: 255607322
dc.identifier.otherPURE UUID: 89198b49-712b-4db6-b6be-f81a200a4abd
dc.identifier.otherRIS: urn:CAC0C176ADB86BD24C4488F998D07BA5
dc.identifier.otherRIS: Mikić2018
dc.identifier.otherScopus: 85056132586
dc.identifier.otherORCID: /0000-0001-6065-8531/work/58055421
dc.identifier.otherWOS: 000448876900022
dc.identifier.urihttp://hdl.handle.net/10023/17180
dc.descriptionD.H.M. thanks both the UK STFC and the Leverhulme Trust for their financial support.en
dc.description.abstractThe total solar eclipse that occurred on 21 August 2017 across the United States provided an opportunity to test a magnetohydrodynamic model of the solar corona driven by measured magnetic fields. We used a new heating model based on the dissipation of Alfvén waves, and a new energization mechanism to twist the magnetic field in filament channels. We predicted what the corona would look like one week before the eclipse. Here, we describe how this prediction was accomplished, and show that it compared favourably with observations of the eclipse in white light and extreme ultraviolet. The model allows us to understand the relationship of observed features, including streamers, coronal holes, prominences, polar plumes and thin rays, to the magnetic field. We show that the discrepancies between the model and observations arise from limitations in our ability to observe the Sun’s magnetic field. Predictions of this kind provide opportunities to improve the models, forging the path to improved space weather prediction.
dc.language.isoeng
dc.relation.ispartofNature Astronomyen
dc.rights© 2018, 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 as such may differ slightly from the final published version. The final published version of this work is available at https://doi.org/10.1038/s41550-018-0562-5en
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectE-NDASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titlePredicting the corona for the 21 August 2017 total solar eclipseen
dc.typeJournal articleen
dc.description.versionPostprinten
dc.contributor.institutionUniversity of St Andrews.Applied Mathematicsen
dc.identifier.doihttps://doi.org/10.1038/s41550-018-0562-5
dc.description.statusPeer revieweden
dc.date.embargoedUntil2019-03-01


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