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dc.contributor.authorReid, Jack
dc.contributor.authorCargill, Peter
dc.contributor.authorHood, Alan William
dc.contributor.authorParnell, Clare Elizabeth
dc.contributor.authorArber, Tony Deane
dc.date.accessioned2019-12-23T10:30:02Z
dc.date.available2019-12-23T10:30:02Z
dc.date.issued2020-01
dc.identifier.citationReid , J , Cargill , P , Hood , A W , Parnell , C E & Arber , T D 2020 , ' Coronal energy release by MHD avalanches : heating mechanisms ' , Astronomy & Astrophysics , vol. 633 , A158 . https://doi.org/10.1051/0004-6361/201937051en
dc.identifier.issn0004-6361
dc.identifier.otherPURE: 264699828
dc.identifier.otherPURE UUID: 5b60b996-6916-4c9b-9b97-89d8169443ba
dc.identifier.otherORCID: /0000-0003-2620-2068/work/68281183
dc.identifier.otherWOS: 000509344300002
dc.identifier.otherORCID: /0000-0002-5694-9069/work/73700701
dc.identifier.otherScopus: 85088696096
dc.identifier.urihttp://hdl.handle.net/10023/19195
dc.descriptionFunding: Carnegie Trust for the Universities of Scotland; Science and Technology Facilities Council (grants ST/N000609/1 and ST/P000320/1).en
dc.description.abstractThe plasma heating associated with an avalanche involving three twisted magnetic threads within a coronal loop is investigated using three-dimensional magnetohydrodynamic simulations. The avalanche is triggered by the kink instability of one thread, with the others being engulfed as a consequence. The heating as a function of both time and location along the strands is evaluated. It is shown to be bursty at all times but to have no preferred spatial location. While there appears to be a level of "background" heating, this is shown to be comprised of individual, small heating events. A comparison between viscous and resistive (Ohmic) heating demonstrates that the strongest heating events are largely associated with the Ohmic heating that arises when the current exceeds a critical value. Viscous heating is largely (but not entirely) associated with smaller events. Ohmic heating dominates viscous heating only at the time of the initial kink instability. It is also demonstrated that a variety of viscous models lead to similar heating rates, suggesting that the system adjusts to dissipate the same amount of energy.
dc.format.extent16
dc.language.isoeng
dc.relation.ispartofAstronomy & Astrophysicsen
dc.rightsCopyright © ESO 2020. This work has been made available online in accordance with publisher policies or with permission. Permission for further reuse of this content should be sought from the publisher or the rights holder. This is the author created accepted manuscript following peer review and may differ slightly from the final published version. The final published version of this work is available at https://doi.org/10.1051/0004-6361/201937051en
dc.subjectSun: coronaen
dc.subjectSun: magnetic fieldsen
dc.subjectMagnetohydrodynamics (MHD)en
dc.subjectMethods: numericalen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectT-NDASen
dc.subjectBDCen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleCoronal energy release by MHD avalanches : heating mechanismsen
dc.typeJournal articleen
dc.description.versionPostprinten
dc.contributor.institutionUniversity of St Andrews.Applied Mathematicsen
dc.contributor.institutionUniversity of St Andrews.School of Mathematics and Statisticsen
dc.identifier.doihttps://doi.org/10.1051/0004-6361/201937051
dc.description.statusPeer revieweden


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