Active region helicity evolution and related coronal mass ejection activity

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The computation of magnetic helicity has become increasingly important in the studies of solar activity. Observations of helical structures in the solar atmosphere, and their subsequent ejection into the interplanetary medium, have resulted in considerable interest to find the link between the amoun...

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Autores principales:	Green, L.M., López Fuentes, M.C., Mandrini, C.H., van Driel-Gesztelyi, L., Démoulin, P.
Formato:	JOUR
Materias:	Magnetic fields Sun Coronal mass ejections (CME) Magnetic helicity Space research corona
Acceso en línea:	http://hdl.handle.net/20.500.12110/paper_02731177_v32_n10_p1959_Green
Aporte de:	Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires

id	todo:paper_02731177_v32_n10_p1959_Green
record_format	dspace
spelling	todo:paper_02731177_v32_n10_p1959_Green2023-10-03T15:15:32Z Active region helicity evolution and related coronal mass ejection activity Green, L.M. López Fuentes, M.C. Mandrini, C.H. van Driel-Gesztelyi, L. Démoulin, P. Magnetic fields Sun Coronal mass ejections (CME) Magnetic helicity Space research corona The computation of magnetic helicity has become increasingly important in the studies of solar activity. Observations of helical structures in the solar atmosphere, and their subsequent ejection into the interplanetary medium, have resulted in considerable interest to find the link between the amount of helicity in the coronal magnetic field and the origin of coronal mass ejections (CMEs), which provide a natural method to remove helicity from the corona. Recent works have endeavored to find the source of helicity to explain the observed CME activity in specific cases. The main candidates being differential rotation, shear motions or a transfer of helicity from below the photosphere into the corona. We study and active region for several rotations during 1997 and 1998 to investigate the relative importance of these mechanisms. We find that photospheric differential rotation cannot provide the required magnetic helicity to the corona and the ejected CMEs. Localized photospheric motions can provide a larger helicity flux, though still not sufficient. © 2003 COSPAR. Published by Elsevier Ltd. All rights reserved. JOUR info:eu-repo/semantics/openAccess http://creativecommons.org/licenses/by/2.5/ar http://hdl.handle.net/20.500.12110/paper_02731177_v32_n10_p1959_Green
institution	Universidad de Buenos Aires
institution_str	I-28
repository_str	R-134
collection	Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA)
topic	Magnetic fields Sun Coronal mass ejections (CME) Magnetic helicity Space research corona
spellingShingle	Magnetic fields Sun Coronal mass ejections (CME) Magnetic helicity Space research corona Green, L.M. López Fuentes, M.C. Mandrini, C.H. van Driel-Gesztelyi, L. Démoulin, P. Active region helicity evolution and related coronal mass ejection activity
topic_facet	Magnetic fields Sun Coronal mass ejections (CME) Magnetic helicity Space research corona
description	The computation of magnetic helicity has become increasingly important in the studies of solar activity. Observations of helical structures in the solar atmosphere, and their subsequent ejection into the interplanetary medium, have resulted in considerable interest to find the link between the amount of helicity in the coronal magnetic field and the origin of coronal mass ejections (CMEs), which provide a natural method to remove helicity from the corona. Recent works have endeavored to find the source of helicity to explain the observed CME activity in specific cases. The main candidates being differential rotation, shear motions or a transfer of helicity from below the photosphere into the corona. We study and active region for several rotations during 1997 and 1998 to investigate the relative importance of these mechanisms. We find that photospheric differential rotation cannot provide the required magnetic helicity to the corona and the ejected CMEs. Localized photospheric motions can provide a larger helicity flux, though still not sufficient. © 2003 COSPAR. Published by Elsevier Ltd. All rights reserved.
format	JOUR
author	Green, L.M. López Fuentes, M.C. Mandrini, C.H. van Driel-Gesztelyi, L. Démoulin, P.
author_facet	Green, L.M. López Fuentes, M.C. Mandrini, C.H. van Driel-Gesztelyi, L. Démoulin, P.
author_sort	Green, L.M.
title	Active region helicity evolution and related coronal mass ejection activity
title_short	Active region helicity evolution and related coronal mass ejection activity
title_full	Active region helicity evolution and related coronal mass ejection activity
title_fullStr	Active region helicity evolution and related coronal mass ejection activity
title_full_unstemmed	Active region helicity evolution and related coronal mass ejection activity
title_sort	active region helicity evolution and related coronal mass ejection activity
url	http://hdl.handle.net/20.500.12110/paper_02731177_v32_n10_p1959_Green
work_keys_str_mv	AT greenlm activeregionhelicityevolutionandrelatedcoronalmassejectionactivity AT lopezfuentesmc activeregionhelicityevolutionandrelatedcoronalmassejectionactivity AT mandrinich activeregionhelicityevolutionandrelatedcoronalmassejectionactivity AT vandrielgesztelyil activeregionhelicityevolutionandrelatedcoronalmassejectionactivity AT demoulinp activeregionhelicityevolutionandrelatedcoronalmassejectionactivity
_version_	1807317910327132160

Active region helicity evolution and related coronal mass ejection activity

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