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dc.contributor.authorPriest, Eric Ronald
dc.contributor.authorLongcope, D W
dc.contributor.authorJanvier, M
dc.date.accessioned2016-08-17T12:30:19Z
dc.date.available2016-08-17T12:30:19Z
dc.date.issued2016-08
dc.identifier.citationPriest , E R , Longcope , D W & Janvier , M 2016 , ' Evolution of magnetic helicity during eruptive flares and coronal mass ejections ' , Solar Physics , vol. 291 , no. 7 , pp. 2017-2036 . https://doi.org/10.1007/s11207-016-0962-6en
dc.identifier.issn0038-0938
dc.identifier.otherPURE: 244841032
dc.identifier.otherPURE UUID: 8c422cd1-968b-47c6-918a-88a818889a7f
dc.identifier.otherScopus: 84982161564
dc.identifier.otherWOS: 000382094000006
dc.identifier.otherORCID: /0000-0003-3621-6690/work/74117722
dc.identifier.urihttps://hdl.handle.net/10023/9320
dc.descriptionFunding: UK STFC, High Altitude Observatory and Montana State University.en
dc.description.abstractDuring eruptive solar flares and coronal mass ejections, a non-potential magnetic arcade with much excess magnetic energy goes unstable and reconnects. It produces a twisted erupting flux rope and leaves behind a sheared arcade of hot coronal loops. We suggest that: the twist of the erupting flux rope can be determined from conservation of magnetic flux and magnetic helicity and equipartition of magnetic helicity. It depends on the geometry of the initial preeruptive structure. Two cases are considered, in the first of which a flux rope is not present initially but is created during the eruption by the reconnection. In the second case, a flux rope is present under the arcade in the pre-eruptive state,and the e.ect of the eruption and reconnection is to add an amount of magnetic helicity that depends on the fluxes of the rope and arcade and the geometry.
dc.format.extent20
dc.language.isoeng
dc.relation.ispartofSolar Physicsen
dc.rights© The Author(s) 2016. This article is published with open access at Springerlink.com This article is distributed under the terms of the Creative Commons Attribution 4.0 International License (http://creativecommons.org/licenses/by/4.0/), 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.subjectSun: flaresen
dc.subjectSun: magnetic topolocyen
dc.subjectMagnetic reconnectionen
dc.subjectHelicityen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectT-NDASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleEvolution of magnetic helicity during eruptive flares and coronal mass ejectionsen
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews. Applied Mathematicsen
dc.identifier.doihttps://doi.org/10.1007/s11207-016-0962-6
dc.description.statusPeer revieweden


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