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dc.contributor.authorBareford, Michael R
dc.contributor.authorGordovskyy, Mykola
dc.contributor.authorBrowning, Philippa
dc.contributor.authorHood, Alan William
dc.date.accessioned2017-12-10T00:31:42Z
dc.date.available2017-12-10T00:31:42Z
dc.date.issued2016-01
dc.identifier.citationBareford , M R , Gordovskyy , M , Browning , P & Hood , A W 2016 , ' Energy release in driven twisted coronal loops ' , Solar Physics , vol. 291 , no. 1 , pp. 187-209 . https://doi.org/10.1007/s11207-015-0824-7en
dc.identifier.issn0038-0938
dc.identifier.otherPURE: 228670817
dc.identifier.otherPURE UUID: 8f577bb0-e273-4d61-ae4f-9ee3f7343692
dc.identifier.otherScopus: 84952629854
dc.identifier.otherORCID: /0000-0003-2620-2068/work/58055162
dc.identifier.otherWOS: 000372878100011
dc.identifier.urihttp://hdl.handle.net/10023/12305
dc.descriptionThis work is funded by Science and Technology Facilities Council (UK). This equipment was funded by a BIS National E-Infrastructure capital grant ST/K00042X/1, DiRAC Operations grant ST/K003267/1 and Durham University.en
dc.description.abstractMagnetic reconnection in twisted magnetic flux tubes, representing coronal loops, is investigated. The main goal is to establish the influence of the field geometry and various thermodynamic effects on the stability of twisted flux tubes and on the size and distribution of heated regions. In particular, we aim to investigate to what extent the earlier idealised models, based on the initially cylindrically symmetric flux tubes, are different from more realistic models, including the large-scale curvature, atmospheric stratification, thermal conduction and other effects. In addition, we compare the roles of Ohmic heating and shock heating in energy conversion during magnetic reconnection in twisted loops. The models with straight flux tubes show similar distribution of heated plasma during the reconnection: it initially forms a helical shape, which subsequently becomes very fragmented. The heating in these models is rather uniformly distributed along flux tubes. At the same time, the hot plasma regions in curved loops are asymmetric, and concentrate close to the loop tops. Large-scale curvature has a destabilising in influence: lower twist is needed for instability. Footpoint convergence normally delays instability slightly, although, in some cases converging flux tubes can be less stable. Finally, introducing a stratified atmosphere gives rise to decaying wave propagation, which has destabilising effect.
dc.format.extent23
dc.language.isoeng
dc.relation.ispartofSolar Physicsen
dc.rights© 2016, Publisher / the Author(s). This work is made available online in accordance with the publisher’s policies. This is the author created, accepted version manuscript following peer review and may differ slightly from the final published version. The final published version of this work is available at link.springer.com / https://dx.doi.org/10.1007/s11207-015-0824-7en
dc.subjectCoronaen
dc.subjectInstabilitiesen
dc.subjectMagnetic fieldsen
dc.subjectMagnetohydrodynamicsen
dc.subjectQB Astronomyen
dc.subjectQA Mathematicsen
dc.subjectQC Physicsen
dc.subjectNDASen
dc.subject.lccQBen
dc.subject.lccQAen
dc.subject.lccQCen
dc.titleEnergy release in driven twisted coronal loopsen
dc.typeJournal articleen
dc.description.versionPostprinten
dc.contributor.institutionUniversity of St Andrews.Applied Mathematicsen
dc.identifier.doihttps://doi.org/10.1007/s11207-015-0824-7
dc.description.statusPeer revieweden
dc.date.embargoedUntil2017-12-09


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