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dc.contributor.authorArchontis, V.
dc.contributor.authorHansteen, V.
dc.date.accessioned2014-09-02T09:31:02Z
dc.date.available2014-09-02T09:31:02Z
dc.date.issued2014-06-10
dc.identifier.citationArchontis , V & Hansteen , V 2014 , ' Clusters of small eruptive flares produced by magnetic reconnection in the Sun ' , Astrophysical Journal Letters , vol. 788 , no. 1 , L2 , pp. 1-6 . https://doi.org/10.1088/2041-8205/788/1/L2en
dc.identifier.issn2041-8205
dc.identifier.otherPURE: 145260976
dc.identifier.otherPURE UUID: a3802f66-967b-4492-9088-66ef70f7059b
dc.identifier.otherScopus: 84901722899
dc.identifier.otherWOS: 000337134100012
dc.identifier.otherORCID: /0000-0002-6926-8676/work/73700866
dc.identifier.urihttp://hdl.handle.net/10023/5316
dc.descriptionThis research was supported by the Research Council of Norway through the grant "Solar Atmospheric Modelling" and through grants of computing time from the Programme for Supercomputing, by the European Research Council under the European Union's Seventh Framework Programme (FP7/2007-2013)/ERC Grant agreement No. 291058 and by computing project s1061 from the High End Computing Division of NASA. The authors acknowledge support by the EU (IEF-272549 grant) and the Royal Society.en
dc.description.abstractWe report on the formation of small solar flares produced by patchy magnetic reconnection between interacting magnetic loops. A three-dimensional (3D) magnetohydrodynamic (MHD) numerical experiment was performed, where a uniform magnetic flux sheet was injected into a fully developed convective layer. The gradual emergence of the field into the solar atmosphere results in a network of magnetic loops, which interact dynamically forming current layers at their interfaces. The formation and ejection of plasmoids out of the current layers leads to patchy reconnection and the spontaneous formation of several small (size ≈1-2 Mm) flares. We find that these flares are short-lived (30 s-3 minutes) bursts of energy in the range O(1025-1027) erg, which is basically the nanoflare-microflare range. Their persistent formation and co-operative action and evolution leads to recurrent emission of fast EUV/X-ray jets and considerable plasma heating in the active corona.
dc.format.extent6
dc.language.isoeng
dc.relation.ispartofAstrophysical Journal Lettersen
dc.rights© 2014. The American Astronomical Society. All rights reserved.en
dc.subjectMagnetohydrodynamics (MHD)en
dc.subjectSun: activityen
dc.subjectSun: coronaen
dc.subjectSun: flaresen
dc.subjectSun: magnetic fieldsen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectBDCen
dc.subjectR2Cen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleClusters of small eruptive flares produced by magnetic reconnection in the Sunen
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews.Applied Mathematicsen
dc.identifier.doihttps://doi.org/10.1088/2041-8205/788/1/L2
dc.description.statusPeer revieweden


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