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dc.contributor.author
Schmieder, B.
dc.contributor.author
Mandrini, Cristina Hemilse
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dc.contributor.author
Démoulin, Pascal
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dc.contributor.author
Pariat, E.
dc.contributor.author
Berlicki, A.
dc.contributor.author
DeLuca, E.
dc.date.available
2017-05-18T19:59:20Z
dc.date.issued
2006-12
dc.identifier.citation
Schmieder, B.; Mandrini, Cristina Hemilse; Démoulin, Pascal; Pariat, E.; Berlicki, A.; et al.; Magnetic reconfiguration before the X17 solar flare of October 28, 2003; Elsevier; Advances In Space Research; 37; 7; 12-2006; 1313-1316
dc.identifier.issn
0273-1177
dc.identifier.uri
http://hdl.handle.net/11336/16675
dc.description.abstract
An active region (AR) NOAA 10486, which produced a large number of X-ray flares during October–November 2003, was observed during a multi-wavelength campaign with ground based and space instruments. We focus our analysis on the observations of October 28, 2003. The magnetic field was observed with THEMIS (Na D1) and MDI (Ni I), the chromosphere with THEMIS (Ca II 8542 A˚ ) and with the Meudon heliograph in Ha, the EUV images with SOHO/EIT and TRACE. Two pre-events started just before the major X 17 flare. One was related to localized flux emergence and lasted until the decay phase of the X flare; while the second one involved a large scale quadrupolar reconnection, that we infer by modeling the AR magnetic field. Extended dimming areas across the equator (EIT), large arcades of post-flare loops (TRACE 195 A˚ ) and a halo CME (LASCO) were observed consequently after the flare. We perform an extrapolation of the magnetic field above the photosphere using a linear force-free-field approximation that allows us to find the connectivity among the four polarities that would be involved in the quadrupolar reconnection event. The X 17 flare is plausibly due to the destabilisation of a twisted flux tube, the bottom part of this magnetic structure
can be visualized by the presence of a filament. The destabilization is caused by converging and shearing photospheric motions towards the main magnetic inversion line. The large scale quadrupolar reconnection related to the second pre-event would favour the opening of the field above the twisted flux tube and, consequently, the coronal mass ejection.
dc.format
application/pdf
dc.language.iso
eng
dc.publisher
Elsevier
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dc.rights
info:eu-repo/semantics/openAccess
dc.rights.uri
https://creativecommons.org/licenses/by-nc-nd/2.5/ar/
dc.subject.classification
Astronomía
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dc.subject.classification
Ciencias Físicas
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dc.subject.classification
CIENCIAS NATURALES Y EXACTAS
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dc.title
Magnetic reconfiguration before the X17 solar flare of October 28, 2003
dc.type
info:eu-repo/semantics/article
dc.type
info:ar-repo/semantics/artículo
dc.type
info:eu-repo/semantics/publishedVersion
dc.date.updated
2017-05-16T15:11:44Z
dc.journal.volume
37
dc.journal.number
7
dc.journal.pagination
1313-1316
dc.journal.pais
Países Bajos
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dc.journal.ciudad
Amsterdam
dc.description.fil
Fil: Schmieder, B.. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia. ITA; Noruega
dc.description.fil
Fil: Mandrini, Cristina Hemilse. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina
dc.description.fil
Fil: Démoulin, Pascal. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia
dc.description.fil
Fil: Pariat, E.. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia
dc.description.fil
Fil: Berlicki, A.. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia
dc.description.fil
Fil: DeLuca, E.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos
dc.journal.title
Advances In Space Research
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dc.relation.alternativeid
info:eu-repo/semantics/altIdentifier/doi/http://dx.doi.org/10.1016/j.asr.2004.12.051
dc.relation.alternativeid
info:eu-repo/semantics/altIdentifier/url/http://www.sciencedirect.com/science/article/pii/S0273117705000360
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