Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/7287
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dc.contributor.authorVemareddy, P-
dc.contributor.authorDemoulin, P-
dc.date.accessioned2018-06-13T05:26:05Z-
dc.date.available2018-06-13T05:26:05Z-
dc.date.issued2018-04-20-
dc.identifier.citationThe Astrophysical Journal, Vol. 857, No. 2, 90en_US
dc.identifier.issn0004-637X-
dc.identifier.urihttp://hdl.handle.net/2248/7287-
dc.descriptionRestricted Accessen_US
dc.description.abstractWe study the magnetic structure of a successively erupting sigmoid in active region 12371 by modeling the quasi-static coronal field evolution with nonlinear force-free field (NLFFF) equilibria. Helioseismic and Magnetic Imager/Solar Dynamic Observatory vector magnetograms are used as input to the NLFFF model. In all eruption events, the modeled structure resembles the observed pre-eruptive coronal sigmoid and the NLFFF core field is a combination of double inverse-J-shaped and inverse-S field lines with dips touching the photosphere. Such field lines are formed by the flux cancellation reconnection of opposite-J field lines at bald-patch locations, which in turn implies the formation of a weakly twisted flux-rope (FR) from large-scale sheared arcade field lines. Later on, this FR undergoes coronal tether-cutting reconnection until a coronal mass ejection is triggered. The modeled structure captured these major features of sigmoid-to-arcade-to-sigmoid transformation, which is reoccuring under continuous photospheric flux motions. Calculations of the field line twist reveal a fractional increase followed by a decrease of the number of pixels having a range of twist. This traces the buildup process of a twisted core field by slow photospheric motions and the relaxation after eruption, respectively. Our study infers that the large eruptivity of this AR is due to a steep decrease of the background coronal field meeting the torus instability criteria at a low height (≈40 Mm) in contrast to noneruptive ARs.en_US
dc.language.isoenen_US
dc.publisherIOP Publishingen_US
dc.relation.urihttps://doi.org/10.3847/1538-4357/aab6b7-
dc.rights© The American Astronomical Society-
dc.subjectSun: coronaen_US
dc.subjectSun: coronal mass ejections (CMEs)en_US
dc.subjectSun: evolutionen_US
dc.subjectSun: filaments, prominencesen_US
dc.subjectSun: flaresen_US
dc.subjectSun: magnetic fieldsen_US
dc.titleStudy of Three-dimensional Magnetic Structure and the Successive Eruptive Nature of Active Region 12371en_US
dc.typeArticleen_US
Appears in Collections:IIAP Publications



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