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dc.contributor.authorPriest, Eric Ronald
dc.contributor.authorLongcope, D.W.
dc.date.accessioned2017-01-16T16:30:13Z
dc.date.available2017-01-16T16:30:13Z
dc.date.issued2017-01
dc.identifier.citationPriest , E R & Longcope , D W 2017 , ' Flux-rope twist in eruptive flares and CMEs : due to zipper and main-phase reconnection ' , Solar Physics , vol. 292 , 25 . https://doi.org/10.1007/s11207-016-1049-0en
dc.identifier.issn0038-0938
dc.identifier.otherPURE: 248657707
dc.identifier.otherPURE UUID: ee9bf71d-52d2-4862-ba15-b6d617a43089
dc.identifier.otherScopus: 85009211878
dc.identifier.otherWOS: 000402763000007
dc.identifier.otherORCID: /0000-0003-3621-6690/work/74117721
dc.identifier.urihttps://hdl.handle.net/10023/10114
dc.descriptionFunding: UK Science and Technology Facilities Councilen
dc.description.abstractThe nature of three-dimensional reconnection when a twisted flux tube erupts during an eruptive flare or coronal mass ejection is considered. The reconnection has two phases: first of all, 3D “zipper reconnection” propagates along the initial coronal arcade, parallel to the polarity inversion line (PIL); then subsequent quasi-2D “main phase reconnection” in the low corona around a flux rope during its eruption produces coronal loops and chromospheric ribbons that propagate away from the PIL in a direction normal to it. One scenario starts with a sheared arcade: the zipper reconnection creates a twisted flux rope of roughly one turn (2π radians of twist), and then main phase reconnection builds up the bulk of the erupting flux rope with a relatively uniform twist of a few turns. A second scenario starts with a pre-existing flux rope under the arcade. Here the zipper phase can create a core with many turns that depend on the ratio of the magnetic fluxes in the newly formed flare ribbons and the new flux rope. Main phase reconnection then adds a layer of roughly uniform twist to the twisted central core. Both phases and scenarios are modeled in a simple way that assumes the initial magnetic flux is fragmented along the PIL. The model uses conservation of magnetic helicity and flux, together with equipartition of magnetic helicity, to deduce the twist of the erupting flux rope in terms the geometry of the initial configuration. Interplanetary observations show some flux ropes have a fairly uniform twist, which could be produced when the zipper phase and any pre-existing flux rope possess small or moderate twist (up to one or two turns). Other interplanetary flux ropes have highly twisted cores (up to five turns), which could be produced when there is a pre-existing flux rope and an active zipper phase that creates substantial extra twist.
dc.format.extent31
dc.language.isoeng
dc.relation.ispartofSolar Physicsen
dc.rightsCopyright the Authors 2017. 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 topologyen
dc.subjectMagnetic reconnectionen
dc.subjectHelicityen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectT-NDASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleFlux-rope twist in eruptive flares and CMEs : due to zipper and main-phase reconnectionen
dc.typeJournal articleen
dc.contributor.sponsorScience & Technology Facilities Councilen
dc.description.versionPostprinten
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews. Applied Mathematicsen
dc.identifier.doihttps://doi.org/10.1007/s11207-016-1049-0
dc.description.statusPeer revieweden
dc.identifier.urlhttp://link.springer.com/article/10.1007/s11207-016-1049-0en
dc.identifier.grantnumberST/K000950/1en


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