Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/7382
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dc.contributor.authorJiang, C-
dc.contributor.authorZou, P-
dc.contributor.authorFeng, X-
dc.contributor.authorHu, Qiang-
dc.contributor.authorLiu, Rui-
dc.contributor.authorVemareddy, P-
dc.contributor.authorDuan, Aiying-
dc.contributor.authorZuo, P-
dc.contributor.authorWang, Yi-
dc.contributor.authorWei, Fengsi-
dc.date.accessioned2019-02-08T10:35:13Z-
dc.date.available2019-02-08T10:35:13Z-
dc.date.issued2018-12-10-
dc.identifier.citationThe Astrophysical Journal, Vol. 869, No.1,13en_US
dc.identifier.issn0004-637X-
dc.identifier.urihttp://hdl.handle.net/2248/7382-
dc.descriptionRestricted Accessen_US
dc.description.abstractThree-dimensional magnetic topology is crucial to understanding the explosive release of magnetic energy in the corona during solar flares. Much attention has been given to the pre-flare magnetic topology to identify candidate sites of magnetic reconnection, yet it is unclear how the magnetic reconnection and its attendant topological changes shape the eruptive structure and how the topology evolves during the eruption. Here we employed a realistic, data-constrained magnetohydrodynamic simulation to study the evolving magnetic topology for an X9.3 eruptive flare that occurred on 2017 September 6. The simulation successfully reproduces the eruptive features and processes in unprecedented detail. The numerical results reveal that the pre-flare corona contains multiple twisted flux systems with different connections, and during the eruption these twisted fluxes form a coherent flux rope through tether-cutting-like magnetic reconnection below the rope. Topological analysis shows that the rising flux rope is wrapped by a quasi-separatrix layer, which intersects itself below the rope, forming a topological structure known as a hyperbolic flux tube, where a current sheet develops, triggering the reconnection. By mapping footpoints of the newly reconnected field lines, we are able to reproduce both the spatial location and, for the first time, the temporal separation of the observed flare ribbons, as well as the dynamic boundary of the flux rope's feet. Furthermore, the temporal profile of the total reconnection flux is comparable to the soft X-ray light curve. Such a sophisticated characterization of the evolving magnetic topology provides important insight into the eventual understanding and forecasting of solar eruptions.en_US
dc.language.isoenen_US
dc.publisherIOP Publishingen_US
dc.relation.urihttps://doi.org/10.3847/1538-4357/aaeacc-
dc.rights© The American Astronomical Society-
dc.subjectMagnetic fieldsen_US
dc.subjectMagnetohydrodynamics (MHD)en_US
dc.subjectMethods: numericalen_US
dc.subjectSun: coronaen_US
dc.subjectSun: flaresen_US
dc.titleMagnetohydrodynamic simulation of the X9.3 flare on 2017 September 6: evolving magnetic topologyen_US
dc.typeArticleen_US
Appears in Collections:IIAP Publications

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