Magnetic reconfiguration before the X 17 Solar flare of October 28 2003

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 T...

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Guardado en:
Detalles Bibliográficos
Publicado: 2006
Materias:
Coronal mass ejection
Sun: flare
Sun: magnetic field
Magnetic fields
Magnetic flux
Solar energy
X rays
Photospheric motions
Space research
Acceso en línea:https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_02731177_v37_n7_p1313_Schmieder
http://hdl.handle.net/20.500.12110/paper_02731177_v37_n7_p1313_Schmieder
Aporte de:
Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires
id paper:paper_02731177_v37_n7_p1313_Schmieder
record_format dspace
spelling paper:paper_02731177_v37_n7_p1313_Schmieder2023-06-08T15:25:35Z Magnetic reconfiguration before the X 17 Solar flare of October 28 2003 Coronal mass ejection Sun: flare Sun: magnetic field Magnetic fields Magnetic flux Solar energy X rays Coronal mass ejection Photospheric motions Sun: flare Sun: magnetic field Space research 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 Å) and with the Meudon heliograph in Hα, 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 Å) 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. © 2005 COSPAR. 2006 https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_02731177_v37_n7_p1313_Schmieder http://hdl.handle.net/20.500.12110/paper_02731177_v37_n7_p1313_Schmieder
institution Universidad de Buenos Aires
institution_str I-28
repository_str R-134
collection Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA)
topic Coronal mass ejection
Sun: flare
Sun: magnetic field
Magnetic fields
Magnetic flux
Solar energy
X rays
Coronal mass ejection
Photospheric motions
Sun: flare
Sun: magnetic field
Space research
spellingShingle Coronal mass ejection
Sun: flare
Sun: magnetic field
Magnetic fields
Magnetic flux
Solar energy
X rays
Coronal mass ejection
Photospheric motions
Sun: flare
Sun: magnetic field
Space research
Magnetic reconfiguration before the X 17 Solar flare of October 28 2003
topic_facet Coronal mass ejection
Sun: flare
Sun: magnetic field
Magnetic fields
Magnetic flux
Solar energy
X rays
Coronal mass ejection
Photospheric motions
Sun: flare
Sun: magnetic field
Space research
description 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 Å) and with the Meudon heliograph in Hα, 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 Å) 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. © 2005 COSPAR.
title Magnetic reconfiguration before the X 17 Solar flare of October 28 2003
title_short Magnetic reconfiguration before the X 17 Solar flare of October 28 2003
title_full Magnetic reconfiguration before the X 17 Solar flare of October 28 2003
title_fullStr Magnetic reconfiguration before the X 17 Solar flare of October 28 2003
title_full_unstemmed Magnetic reconfiguration before the X 17 Solar flare of October 28 2003
title_sort magnetic reconfiguration before the x 17 solar flare of october 28 2003
publishDate 2006
url https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_02731177_v37_n7_p1313_Schmieder
http://hdl.handle.net/20.500.12110/paper_02731177_v37_n7_p1313_Schmieder
_version_ 1768543228370354176

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