Solar activity due to magnetic complexity of active regions

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Active regions (ARs), involved in the Halloween events during October-November 2003, were the source of unusual activity during the following solar rotation. The flares on 18-20 November 2003 that occur in the AR NOAA10501 were accompanied by coronal mass ejections associated to some particularly ge...

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Autores principales:	Schmieder, B., Mandrini, C., Chandra, R., Démoulin, P., Török, T., Pariat, E., Uddin, W.
Formato:	Artículo publishedVersion
Lenguaje:	Inglés
Publicado:	2010
Materias:	Active region Filament reconnection Magnetic helicity
Acceso en línea:	http://hdl.handle.net/20.500.12110/paper_17439213_v6_nS273_p164_Schmieder
Aporte de:	Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires

id	paperaa:paper_17439213_v6_nS273_p164_Schmieder
record_format	dspace
spelling	paperaa:paper_17439213_v6_nS273_p164_Schmieder2023-06-12T16:51:12Z Solar activity due to magnetic complexity of active regions Proc. Int. Astron. Union 2010;6(S273):164-168 Schmieder, B. Mandrini, C. Chandra, R. Démoulin, P. Török, T. Pariat, E. Uddin, W. Active region Filament reconnection Magnetic helicity Active regions (ARs), involved in the Halloween events during October-November 2003, were the source of unusual activity during the following solar rotation. The flares on 18-20 November 2003 that occur in the AR NOAA10501 were accompanied by coronal mass ejections associated to some particularly geoeffective magnetic clouds. Our analysis of the magnetic flux and helicity injection revealed that a new emerging bipole and consequent shearing motions continuously energized the region during its disk passage. The stored energy was eventually released through the interaction of the various systems of magnetic loops by several magnetic reconnection events. Active events on November 18 (filament eruptions and CMEs) were originated by shearing motions along a section of the filament channel that injected magnetic helicity with sign opposite to that of the AR. Two homologous flares, that occurred on November 20, were apparently triggered by different mechanisms as inferred from the flare ribbons evolution (filament eruption and CMEs). We studied in detail the behaviour of two North-South oriented filaments on November 20 2003. They merged and split following a process suggestive of 'sling-shot' reconnection between two coronal flux ropes. We successfully tested this scenario in a 3D MHD simulation that is presented in this paper. © International Astronomical Union 2011. Fil:Mandrini, C. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina. 2010 info:eu-repo/semantics/article info:ar-repo/semantics/artículo info:eu-repo/semantics/publishedVersion application/pdf eng info:eu-repo/semantics/openAccess http://creativecommons.org/licenses/by/2.5/ar http://hdl.handle.net/20.500.12110/paper_17439213_v6_nS273_p164_Schmieder
institution	Universidad de Buenos Aires
institution_str	I-28
repository_str	R-134
collection	Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA)
language	Inglés
orig_language_str_mv	eng
topic	Active region Filament reconnection Magnetic helicity
spellingShingle	Active region Filament reconnection Magnetic helicity Schmieder, B. Mandrini, C. Chandra, R. Démoulin, P. Török, T. Pariat, E. Uddin, W. Solar activity due to magnetic complexity of active regions
topic_facet	Active region Filament reconnection Magnetic helicity
description	Active regions (ARs), involved in the Halloween events during October-November 2003, were the source of unusual activity during the following solar rotation. The flares on 18-20 November 2003 that occur in the AR NOAA10501 were accompanied by coronal mass ejections associated to some particularly geoeffective magnetic clouds. Our analysis of the magnetic flux and helicity injection revealed that a new emerging bipole and consequent shearing motions continuously energized the region during its disk passage. The stored energy was eventually released through the interaction of the various systems of magnetic loops by several magnetic reconnection events. Active events on November 18 (filament eruptions and CMEs) were originated by shearing motions along a section of the filament channel that injected magnetic helicity with sign opposite to that of the AR. Two homologous flares, that occurred on November 20, were apparently triggered by different mechanisms as inferred from the flare ribbons evolution (filament eruption and CMEs). We studied in detail the behaviour of two North-South oriented filaments on November 20 2003. They merged and split following a process suggestive of 'sling-shot' reconnection between two coronal flux ropes. We successfully tested this scenario in a 3D MHD simulation that is presented in this paper. © International Astronomical Union 2011.
format	Artículo Artículo publishedVersion
author	Schmieder, B. Mandrini, C. Chandra, R. Démoulin, P. Török, T. Pariat, E. Uddin, W.
author_facet	Schmieder, B. Mandrini, C. Chandra, R. Démoulin, P. Török, T. Pariat, E. Uddin, W.
author_sort	Schmieder, B.
title	Solar activity due to magnetic complexity of active regions
title_short	Solar activity due to magnetic complexity of active regions
title_full	Solar activity due to magnetic complexity of active regions
title_fullStr	Solar activity due to magnetic complexity of active regions
title_full_unstemmed	Solar activity due to magnetic complexity of active regions
title_sort	solar activity due to magnetic complexity of active regions
publishDate	2010
url	http://hdl.handle.net/20.500.12110/paper_17439213_v6_nS273_p164_Schmieder
work_keys_str_mv	AT schmiederb solaractivityduetomagneticcomplexityofactiveregions AT mandrinic solaractivityduetomagneticcomplexityofactiveregions AT chandrar solaractivityduetomagneticcomplexityofactiveregions AT demoulinp solaractivityduetomagneticcomplexityofactiveregions AT torokt solaractivityduetomagneticcomplexityofactiveregions AT pariate solaractivityduetomagneticcomplexityofactiveregions AT uddinw solaractivityduetomagneticcomplexityofactiveregions
_version_	1769810144926892032

Solar activity due to magnetic complexity of active regions

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