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dc.contributor.authorLi, Y.
dc.contributor.authorSun, X.
dc.contributor.authorDing, M. D.
dc.contributor.authorQiu, J.
dc.contributor.authorPriest, E. R.
dc.identifier.citationLi , Y , Sun , X , Ding , M D , Qiu , J & Priest , E R 2017 , ' Imaging observations of magnetic reconnection in a solar eruptive flare ' , Astrophysical Journal , vol. 835 , no. 2 , 190 .
dc.identifier.otherPURE: 249407642
dc.identifier.otherPURE UUID: 4f62d461-6662-4ed5-9594-ca6b91f9e4b0
dc.identifier.otherScopus: 85012014200
dc.identifier.otherWOS: 000401145700006
dc.identifier.otherORCID: /0000-0003-3621-6690/work/74117702
dc.description.abstractSolar flares are among the most energetic events in the solar atmosphere. It is widely accepted that flares are powered by magnetic reconnection in the corona. An eruptive flare is usually accompanied by a coronal mass ejection, both of which are probably driven by the eruption of a magnetic flux rope (MFR). Here we report an eruptive flare on 2016 March 23 observed by the Atmospheric Imaging Assembly on board the Solar Dynamics Observatory. The extreme-ultraviolet imaging observations exhibit the clear rise and eruption of an MFR. In particular, the observations reveal solid evidence of magnetic reconnection from both the corona and chromosphere during the flare. Moreover, weak reconnection is observed before the start of the flare. We find that the preflare weak reconnection is of tether-cutting type and helps the MFR to rise slowly. Induced by a further rise of the MFR, strong reconnection occurs in the rise phases of the flare, which is temporally related to the MFR eruption. We also find that the magnetic reconnection is more of 3D-type in the early phase, as manifested in a strong-to-weak shear transition in flare loops, and becomes more 2D-like in the later phase, as shown by the apparent rising motion of an arcade of flare loops.
dc.relation.ispartofAstrophysical Journalen
dc.rights© 2017 The American Astronomical Society. All rights reserved. This work is made available online in accordance with the publisher’s policies. This is the final published version of the work, which was originally published at:
dc.subjectMagnetic reconnectionen
dc.subjectSun: activityen
dc.subjectSun: flaresen
dc.subjectSun: UV radiationen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectAstronomy and Astrophysicsen
dc.subjectSpace and Planetary Scienceen
dc.titleImaging observations of magnetic reconnection in a solar eruptive flareen
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews. School of Mathematics and Statisticsen
dc.contributor.institutionUniversity of St Andrews. Applied Mathematicsen
dc.description.statusPeer revieweden

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