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Evolution of magnetic helicity during eruptive flares and coronal mass ejections
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dc.contributor.author | Priest, Eric Ronald | |
dc.contributor.author | Longcope, D W | |
dc.contributor.author | Janvier, M | |
dc.date.accessioned | 2016-08-17T12:30:19Z | |
dc.date.available | 2016-08-17T12:30:19Z | |
dc.date.issued | 2016-08 | |
dc.identifier.citation | Priest , 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/s11207-016-0962-6 | en |
dc.identifier.issn | 0038-0938 | |
dc.identifier.other | PURE: 244841032 | |
dc.identifier.other | PURE UUID: 8c422cd1-968b-47c6-918a-88a818889a7f | |
dc.identifier.other | Scopus: 84982161564 | |
dc.identifier.other | WOS: 000382094000006 | |
dc.identifier.other | ORCID: /0000-0003-3621-6690/work/74117722 | |
dc.identifier.uri | https://hdl.handle.net/10023/9320 | |
dc.description | Funding: UK STFC, High Altitude Observatory and Montana State University. | en |
dc.description.abstract | During 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.extent | 20 | |
dc.language.iso | eng | |
dc.relation.ispartof | Solar Physics | en |
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.subject | Sun: flares | en |
dc.subject | Sun: magnetic topolocy | en |
dc.subject | Magnetic reconnection | en |
dc.subject | Helicity | en |
dc.subject | QB Astronomy | en |
dc.subject | QC Physics | en |
dc.subject | T-NDAS | en |
dc.subject.lcc | QB | en |
dc.subject.lcc | QC | en |
dc.title | Evolution of magnetic helicity during eruptive flares and coronal mass ejections | en |
dc.type | Journal article | en |
dc.description.version | Publisher PDF | en |
dc.contributor.institution | University of St Andrews. Applied Mathematics | en |
dc.identifier.doi | https://doi.org/10.1007/s11207-016-0962-6 | |
dc.description.status | Peer reviewed | en |
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