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dc.contributor.authorSun, J.Q.
dc.contributor.authorCheng, X.
dc.contributor.authorDing, M.D.
dc.contributor.authorGuo, Y.
dc.contributor.authorPriest, E.R.
dc.contributor.authorParnell, C.E.
dc.contributor.authorEdwards, S.J.
dc.contributor.authorZhang, J.
dc.contributor.authorChen, P.F.
dc.contributor.authorFang, C.
dc.date.accessioned2015-07-24T11:10:04Z
dc.date.available2015-07-24T11:10:04Z
dc.date.issued2015-06-26
dc.identifier.citationSun , J Q , Cheng , X , Ding , M D , Guo , Y , Priest , E R , Parnell , C E , Edwards , S J , Zhang , J , Chen , P F & Fang , C 2015 , ' Extreme ultraviolet imaging of three-dimensional magnetic reconnection in a solar eruption ' , Nature Communications , vol. 6 , 7598 . https://doi.org/10.1038/ncomms8598en
dc.identifier.issn2041-1723
dc.identifier.otherPURE: 204816843
dc.identifier.otherPURE UUID: a88b7983-9588-4d68-b675-6d89d3413c42
dc.identifier.otherScopus: 84933558005
dc.identifier.otherWOS: 000357181700001
dc.identifier.otherORCID: /0000-0002-5694-9069/work/73700708
dc.identifier.otherORCID: /0000-0003-3621-6690/work/74117706
dc.identifier.urihttp://hdl.handle.net/10023/7025
dc.descriptionX.C., J.Q.S., M.D.D., Y.G., P.F.C. and C.F. are supported by NSFC through grants 11303016, 11373023, 11203014 and 11025314, and by NKBRSF through grants 2011CB811402 and 2014CB744203. C.E.P. and S.J.E. are supported by the UK STFC. J.Z. is supported by US NSF AGS-1249270 and AGS-1156120.en
dc.description.abstractMagnetic reconnection, a change of magnetic field connectivity, is a fundamental physical process in which magnetic energy is released explosively, and it is responsible for various eruptive phenomena in the universe. However, this process is difficult to observe directly. Here, the magnetic topology associated with a solar reconnection event is studied in three dimensions using the combined perspectives of two spacecraft. The sequence of extreme ultraviolet images clearly shows that two groups of oppositely directed and non-coplanar magnetic loops gradually approach each other, forming a separator or quasi-separator and then reconnecting. The plasma near the reconnection site is subsequently heated from ∼ 1 to ≥ 5MK. Shortly afterwards, warm flare loops (∼3MK) appear underneath the hot plasma. Other observational signatures of reconnection, including plasma inflows and downflows, are unambiguously revealed and quantitatively measured. These observations provide direct evidence of magnetic reconnection in a three-dimensional configuration and reveal its origin.
dc.language.isoeng
dc.relation.ispartofNature Communicationsen
dc.rightsCopyright 2015 the Authors. This work is licensed under a Creative Commons Attribution 4.0 International License. The images or other third party material in this article are included in the article’s Creative Commons license, unless indicated otherwise in the credit line; if the material is not included under the Creative Commons license, users will need to obtain permission from the license holder to reproduce the material. To view a copy of this license, visit http://creativecommons.org/licenses/by/4.0/en
dc.subjectQC Physicsen
dc.subjectQA Mathematicsen
dc.subjectNDASen
dc.subject.lccQCen
dc.subject.lccQAen
dc.titleExtreme ultraviolet imaging of three-dimensional magnetic reconnection in a solar eruptionen
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews.Applied Mathematicsen
dc.identifier.doihttps://doi.org/10.1038/ncomms8598
dc.description.statusPeer revieweden
dc.identifier.urlhttp://www.nature.com/ncomms/2015/150626/ncomms8598/full/ncomms8598.html#supplementary-informationen


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