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dc.contributor.authorSyntelis, P.
dc.contributor.authorLee, E. J.
dc.contributor.authorFairbairn, C. W.
dc.contributor.authorArchontis, V.
dc.contributor.authorHood, A. W.
dc.date.accessioned2019-09-23T09:30:05Z
dc.date.available2019-09-23T09:30:05Z
dc.date.issued2019-10
dc.identifier.citationSyntelis , P , Lee , E J , Fairbairn , C W , Archontis , V & Hood , A W 2019 , ' Eruptions and flaring activity in emerging quadrupolar regions ' , Astronomy & Astrophysics , vol. 630 , A134 , pp. 1-14 . https://doi.org/10.1051/0004-6361/201936246en
dc.identifier.issn0004-6361
dc.identifier.otherPURE: 261287231
dc.identifier.otherPURE UUID: 5c541685-4556-493e-b4e6-ea4fa0c7d85c
dc.identifier.otherBibCode: 2019arXiv190901446S
dc.identifier.otherORCID: /0000-0003-2620-2068/work/64033770
dc.identifier.otherScopus: 85073190052
dc.identifier.otherWOS: 000516617400007
dc.identifier.otherORCID: /0000-0002-6926-8676/work/73700869
dc.identifier.otherORCID: /0000-0002-6377-0243/work/77131786
dc.identifier.urihttps://hdl.handle.net/10023/18536
dc.descriptionFunding: UK Science and Technology Facilities Council (UK) through the consolidated grant ST/S000402/1, Royal Society grant RGF/EA/180232, ERC synergy grant “The Whole Sun”.en
dc.description.abstractContext. Solar observations suggest that some of the most dynamic active regions are associated with complex photospheric magnetic configurations such as quadrupolar regions, and especially those that have a δ-spot configuration and a strong polarity inversion line (PIL). Aims. We study the formation and eruption of magnetic flux ropes in quadrupolar regions. Methods. We performed 3D magnetohydrodynamics simulations of the partial emergence of a highly twisted flux tube from the solar interior into a non-magnetised stratified atmosphere. We introduced a density deficit at two places along the length of the subphotospheric flux tube to emerge as two Ω-shaped loops, forming a quadrupolar region. Results. At the photosphere, the emerging flux forms two initially separated bipoles, which later come in contact, forming a δ-spot central region. Above the two bipoles, two magnetic lobes expand and interact through a series of current sheets at the interface between them. Two recurrent confined eruptions are produced. In both cases, the reconnection between sheared low-lying field lines forms a flux rope. The reconnection between the two lobes higher in the atmosphere forms field lines that retract down and push against the flux rope, creating a current sheet between them. It also forms field lines that create a third magnetic lobe between the two emerged lobes, that later acts as a strapping field. The flux rope eruptions are triggered when the reconnection between the flux ropes and the field above the ropes becomes efficient enough to remove the tension of the overlying field. These reconnection events occur internally in the quadrupolar system, as the atmosphere is non-magnetised. The flux rope of the first, weaker, eruption almost fully reconnects with the overlying field. The flux rope of the second, more energetic, eruption is confined by the overlying strapping field. During the second eruption, the flux rope is enhanced in size, flux, and twist, similar to confined-flare-to-flux-rope observations. Proxies of the emission reveal the two erupting filaments channels. A flare arcade is only formed in the second eruption owing to the longer lasting and more efficient reconnection at the current sheet below the flux rope.
dc.format.extent14
dc.language.isoeng
dc.relation.ispartofAstronomy & Astrophysicsen
dc.rightsCopyright © 2019 ESO. 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/10.1051/0004-6361/201936246en
dc.subjectSun: activityen
dc.subjectSun: coronaen
dc.subjectSun: magnetic fieldsen
dc.subjectMagnetohydrodynamics (MHD)en
dc.subjectMethods: numericalen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectNDASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleEruptions and flaring activity in emerging quadrupolar regionsen
dc.typeJournal articleen
dc.contributor.sponsorScience & Technology Facilities Councilen
dc.contributor.sponsorScience & Technology Facilities Councilen
dc.contributor.sponsorThe Royal Societyen
dc.contributor.sponsorEuropean Research Councilen
dc.description.versionPostprinten
dc.contributor.institutionUniversity of St Andrews. Applied Mathematicsen
dc.identifier.doihttps://doi.org/10.1051/0004-6361/201936246
dc.description.statusPeer revieweden
dc.identifier.urlhttp://adsabs.harvard.edu/abs/2019arXiv190901446Sen
dc.identifier.grantnumberST/S000402/1en
dc.identifier.grantnumberST/N000609/1en
dc.identifier.grantnumberRGF/EA/180232en
dc.identifier.grantnumber810218en


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