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: Mandrini, Cristina Hemilse, Dasso, Sergio Ricardo
Publicado: 2007
Acceso en línea:https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00380938_v244_n1-2_p95_Harra
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
id paper:paper_00380938_v244_n1-2_p95_Harra
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spelling paper:paper_00380938_v244_n1-2_p95_Harra2023-06-08T15:02:42Z How does large flaring activity from the same active region produce oppositely directed magnetic clouds? Mandrini, Cristina Hemilse Dasso, Sergio Ricardo 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. 2007 https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00380938_v244_n1-2_p95_Harra 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.
author Mandrini, Cristina Hemilse
Dasso, Sergio Ricardo
spellingShingle Mandrini, Cristina Hemilse
Dasso, Sergio Ricardo
How does large flaring activity from the same active region produce oppositely directed magnetic clouds?
author_facet Mandrini, Cristina Hemilse
Dasso, Sergio Ricardo
author_sort Mandrini, Cristina Hemilse
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?
publishDate 2007
url https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00380938_v244_n1-2_p95_Harra
http://hdl.handle.net/20.500.12110/paper_00380938_v244_n1-2_p95_Harra
work_keys_str_mv AT mandrinicristinahemilse howdoeslargeflaringactivityfromthesameactiveregionproduceoppositelydirectedmagneticclouds
AT dassosergioricardo howdoeslargeflaringactivityfromthesameactiveregionproduceoppositelydirectedmagneticclouds
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