How does large flaring activity from the same active region produce oppositely directed magnetic clouds?

We describe the interplanetary coronal mass ejections (ICMEs) that occurred as a result of a series of solar flares and eruptions from 4 to 8 November 2004. Two ICMEs/magnetic clouds occurring from these events had opposite magnetic orientations. This was despite the fact that the major flares relat...

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Autores principales: Harra, L.K., Crooker, N.U., Mandrini, C.H., Van Driel-Gesztelyi, L., Dasso, S., Wang, J., Elliott, H., Attrill, G., Jackson, B.V., Bisi, M.M.
Formato: JOUR
Acceso en línea:http://hdl.handle.net/20.500.12110/paper_00380938_v244_n1-2_p95_Harra
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Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires
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spelling todo:paper_00380938_v244_n1-2_p95_Harra2023-10-03T14:48:39Z How does large flaring activity from the same active region produce oppositely directed magnetic clouds? Harra, L.K. Crooker, N.U. Mandrini, C.H. Van Driel-Gesztelyi, L. Dasso, S. Wang, J. Elliott, H. Attrill, G. Jackson, B.V. Bisi, M.M. We describe the interplanetary coronal mass ejections (ICMEs) that occurred as a result of a series of solar flares and eruptions from 4 to 8 November 2004. Two ICMEs/magnetic clouds occurring from these events had opposite magnetic orientations. This was despite the fact that the major flares related to these events occurred within the same active region that maintained the same magnetic configuration. The solar events include a wide array of activities: flares, trans-equatorial coronal loop disappearance and reformation, trans-equatorial filament eruption, and coronal hole interaction. The first major ICME/magnetic cloud was predominantly related to the active region 10696 eruption. The second major ICME/magnetic cloud was found to be consistent with the magnetic orientation of an erupting trans-equatorial filament or else a rotation of 160° of a flux rope in the active region. We discuss these possibilities and emphasize the importance of understanding the magnetic evolution of the solar source region before we can begin to predict geoeffective events with any accuracy. © 2007 Springer Science+Business Media B.V. Fil:Mandrini, C.H. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina. Fil:Dasso, S. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina. JOUR info:eu-repo/semantics/openAccess http://creativecommons.org/licenses/by/2.5/ar http://hdl.handle.net/20.500.12110/paper_00380938_v244_n1-2_p95_Harra
institution Universidad de Buenos Aires
institution_str I-28
repository_str R-134
collection Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA)
description We describe the interplanetary coronal mass ejections (ICMEs) that occurred as a result of a series of solar flares and eruptions from 4 to 8 November 2004. Two ICMEs/magnetic clouds occurring from these events had opposite magnetic orientations. This was despite the fact that the major flares related to these events occurred within the same active region that maintained the same magnetic configuration. The solar events include a wide array of activities: flares, trans-equatorial coronal loop disappearance and reformation, trans-equatorial filament eruption, and coronal hole interaction. The first major ICME/magnetic cloud was predominantly related to the active region 10696 eruption. The second major ICME/magnetic cloud was found to be consistent with the magnetic orientation of an erupting trans-equatorial filament or else a rotation of 160° of a flux rope in the active region. We discuss these possibilities and emphasize the importance of understanding the magnetic evolution of the solar source region before we can begin to predict geoeffective events with any accuracy. © 2007 Springer Science+Business Media B.V.
format JOUR
author Harra, L.K.
Crooker, N.U.
Mandrini, C.H.
Van Driel-Gesztelyi, L.
Dasso, S.
Wang, J.
Elliott, H.
Attrill, G.
Jackson, B.V.
Bisi, M.M.
spellingShingle Harra, L.K.
Crooker, N.U.
Mandrini, C.H.
Van Driel-Gesztelyi, L.
Dasso, S.
Wang, J.
Elliott, H.
Attrill, G.
Jackson, B.V.
Bisi, M.M.
How does large flaring activity from the same active region produce oppositely directed magnetic clouds?
author_facet Harra, L.K.
Crooker, N.U.
Mandrini, C.H.
Van Driel-Gesztelyi, L.
Dasso, S.
Wang, J.
Elliott, H.
Attrill, G.
Jackson, B.V.
Bisi, M.M.
author_sort Harra, L.K.
title How does large flaring activity from the same active region produce oppositely directed magnetic clouds?
title_short How does large flaring activity from the same active region produce oppositely directed magnetic clouds?
title_full How does large flaring activity from the same active region produce oppositely directed magnetic clouds?
title_fullStr How does large flaring activity from the same active region produce oppositely directed magnetic clouds?
title_full_unstemmed How does large flaring activity from the same active region produce oppositely directed magnetic clouds?
title_sort how does large flaring activity from the same active region produce oppositely directed magnetic clouds?
url http://hdl.handle.net/20.500.12110/paper_00380938_v244_n1-2_p95_Harra
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