What is the source of the magnetic helicity shed by CMEs? The long-term helicity budget of AR 7978

Autores
Démoulin, Pascal; Mandrini, Cristina Hemilse; van Driel Gesztelyi, Lidia; Thompson, B. J.; Plunkett, S.; Kovári, Zs.; Aulanier, G.; Young, A.
Año de publicación
2002
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
An isolated active region (AR) was observed on the Sun during seven rotations, starting from its birth in July 1996 to its full dispersion in December 1996. We analyse the long-term budget of the AR relative magnetic helicity. Firstly, we calculate the helicity injected by differential rotation at the photospheric level using MDI/SoHO magnetograms. Secondly, we compute the coronal magnetic field and its helicity selecting the model which best fits the soft X-ray loops observed with SXT/Yohkoh. Finally, we identify all the coronal mass ejections (CMEs) that originated from the AR during its lifetime using LASCO and EIT/SoHO. Assuming a one to one correspondence between CMEs and magnetic clouds, we estimate the magnetic helicity which could be shed via CMEs. We find that differential rotation can neither provide the required magnetic helicity to the coronal field (at least a factor 2.5 to 4 larger), nor to the field ejected to the interplanetary space (a factor 4 to 20 larger), even in the case of this AR for which the total helicity injected by differential rotation is close to the maximum possible value. However, the total helicity ejected is equivalent to that of a twisted flux tube having the same magnetic flux as the studied AR and a number of turns in the interval [0.5,2.0]. We suggest that the main source of helicity is the inherent twist of the magnetic flux tube forming the active region. This magnetic helicity is transferred to the corona either by the continuous emergence of the flux tube for several solar rotations (i.e. on a time scale much longer than the classical emergence phase), or by torsional Alfvén waves.
Fil: Démoulin, Pascal. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia
Fil: Mandrini, Cristina Hemilse. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina
Fil: van Driel Gesztelyi, Lidia. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia
Fil: Thompson, B. J.. National Aeronautics and Space Administration. Goddart Institute for Space Studies; Estados Unidos
Fil: Plunkett, S.. Spece Sciences División. Naval Research Laboratory; Estados Unidos
Fil: Kovári, Zs.. Konkoly Observatory; Hungría
Fil: Aulanier, G.. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia
Fil: Young, A.. National Aeronautics and Space Administration. Goddart Institute for Space Studies; Estados Unidos
Materia
SOLAR CORONA
CORONAL MASS EJECTIONS
SOLAR MAGNETIC FIELDS
SOLAR-TERRESTRIAL RELATIONS
Nivel de accesibilidad
acceso abierto
Condiciones de uso
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
Repositorio
CONICET Digital (CONICET)
Institución
Consejo Nacional de Investigaciones Científicas y Técnicas
OAI Identificador
oai:ri.conicet.gov.ar:11336/22443

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network_name_str CONICET Digital (CONICET)
spelling What is the source of the magnetic helicity shed by CMEs? The long-term helicity budget of AR 7978Démoulin, PascalMandrini, Cristina Hemilsevan Driel Gesztelyi, LidiaThompson, B. J.Plunkett, S.Kovári, Zs.Aulanier, G.Young, A.SOLAR CORONACORONAL MASS EJECTIONSSOLAR MAGNETIC FIELDSSOLAR-TERRESTRIAL RELATIONShttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1An isolated active region (AR) was observed on the Sun during seven rotations, starting from its birth in July 1996 to its full dispersion in December 1996. We analyse the long-term budget of the AR relative magnetic helicity. Firstly, we calculate the helicity injected by differential rotation at the photospheric level using MDI/SoHO magnetograms. Secondly, we compute the coronal magnetic field and its helicity selecting the model which best fits the soft X-ray loops observed with SXT/Yohkoh. Finally, we identify all the coronal mass ejections (CMEs) that originated from the AR during its lifetime using LASCO and EIT/SoHO. Assuming a one to one correspondence between CMEs and magnetic clouds, we estimate the magnetic helicity which could be shed via CMEs. We find that differential rotation can neither provide the required magnetic helicity to the coronal field (at least a factor 2.5 to 4 larger), nor to the field ejected to the interplanetary space (a factor 4 to 20 larger), even in the case of this AR for which the total helicity injected by differential rotation is close to the maximum possible value. However, the total helicity ejected is equivalent to that of a twisted flux tube having the same magnetic flux as the studied AR and a number of turns in the interval [0.5,2.0]. We suggest that the main source of helicity is the inherent twist of the magnetic flux tube forming the active region. This magnetic helicity is transferred to the corona either by the continuous emergence of the flux tube for several solar rotations (i.e. on a time scale much longer than the classical emergence phase), or by torsional Alfvén waves.Fil: Démoulin, Pascal. Centre National de la Recherche Scientifique. Observatoire de Paris; FranciaFil: Mandrini, Cristina Hemilse. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; ArgentinaFil: van Driel Gesztelyi, Lidia. Centre National de la Recherche Scientifique. Observatoire de Paris; FranciaFil: Thompson, B. J.. National Aeronautics and Space Administration. Goddart Institute for Space Studies; Estados UnidosFil: Plunkett, S.. Spece Sciences División. Naval Research Laboratory; Estados UnidosFil: Kovári, Zs.. Konkoly Observatory; HungríaFil: Aulanier, G.. Centre National de la Recherche Scientifique. Observatoire de Paris; FranciaFil: Young, A.. National Aeronautics and Space Administration. Goddart Institute for Space Studies; Estados UnidosEDP Sciences2002-02info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/22443Démoulin, Pascal; Mandrini, Cristina Hemilse; van Driel Gesztelyi, Lidia; Thompson, B. J.; Plunkett, S.; et al.; What is the source of the magnetic helicity shed by CMEs? The long-term helicity budget of AR 7978; EDP Sciences; Astronomy and Astrophysics; 382; 2; 2-2002; 650-6650004-6361CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361:20011634info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/abs/2002/05/aa1962/aa1962.htmlinfo:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T09:59:16Zoai:ri.conicet.gov.ar:11336/22443instacron:CONICETInstitucionalhttp://ri.conicet.gov.ar/Organismo científico-tecnológicoNo correspondehttp://ri.conicet.gov.ar/oai/requestdasensio@conicet.gov.ar; lcarlino@conicet.gov.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:34982025-09-29 09:59:16.659CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv What is the source of the magnetic helicity shed by CMEs? The long-term helicity budget of AR 7978
title What is the source of the magnetic helicity shed by CMEs? The long-term helicity budget of AR 7978
spellingShingle What is the source of the magnetic helicity shed by CMEs? The long-term helicity budget of AR 7978
Démoulin, Pascal
SOLAR CORONA
CORONAL MASS EJECTIONS
SOLAR MAGNETIC FIELDS
SOLAR-TERRESTRIAL RELATIONS
title_short What is the source of the magnetic helicity shed by CMEs? The long-term helicity budget of AR 7978
title_full What is the source of the magnetic helicity shed by CMEs? The long-term helicity budget of AR 7978
title_fullStr What is the source of the magnetic helicity shed by CMEs? The long-term helicity budget of AR 7978
title_full_unstemmed What is the source of the magnetic helicity shed by CMEs? The long-term helicity budget of AR 7978
title_sort What is the source of the magnetic helicity shed by CMEs? The long-term helicity budget of AR 7978
dc.creator.none.fl_str_mv Démoulin, Pascal
Mandrini, Cristina Hemilse
van Driel Gesztelyi, Lidia
Thompson, B. J.
Plunkett, S.
Kovári, Zs.
Aulanier, G.
Young, A.
author Démoulin, Pascal
author_facet Démoulin, Pascal
Mandrini, Cristina Hemilse
van Driel Gesztelyi, Lidia
Thompson, B. J.
Plunkett, S.
Kovári, Zs.
Aulanier, G.
Young, A.
author_role author
author2 Mandrini, Cristina Hemilse
van Driel Gesztelyi, Lidia
Thompson, B. J.
Plunkett, S.
Kovári, Zs.
Aulanier, G.
Young, A.
author2_role author
author
author
author
author
author
author
dc.subject.none.fl_str_mv SOLAR CORONA
CORONAL MASS EJECTIONS
SOLAR MAGNETIC FIELDS
SOLAR-TERRESTRIAL RELATIONS
topic SOLAR CORONA
CORONAL MASS EJECTIONS
SOLAR MAGNETIC FIELDS
SOLAR-TERRESTRIAL RELATIONS
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv An isolated active region (AR) was observed on the Sun during seven rotations, starting from its birth in July 1996 to its full dispersion in December 1996. We analyse the long-term budget of the AR relative magnetic helicity. Firstly, we calculate the helicity injected by differential rotation at the photospheric level using MDI/SoHO magnetograms. Secondly, we compute the coronal magnetic field and its helicity selecting the model which best fits the soft X-ray loops observed with SXT/Yohkoh. Finally, we identify all the coronal mass ejections (CMEs) that originated from the AR during its lifetime using LASCO and EIT/SoHO. Assuming a one to one correspondence between CMEs and magnetic clouds, we estimate the magnetic helicity which could be shed via CMEs. We find that differential rotation can neither provide the required magnetic helicity to the coronal field (at least a factor 2.5 to 4 larger), nor to the field ejected to the interplanetary space (a factor 4 to 20 larger), even in the case of this AR for which the total helicity injected by differential rotation is close to the maximum possible value. However, the total helicity ejected is equivalent to that of a twisted flux tube having the same magnetic flux as the studied AR and a number of turns in the interval [0.5,2.0]. We suggest that the main source of helicity is the inherent twist of the magnetic flux tube forming the active region. This magnetic helicity is transferred to the corona either by the continuous emergence of the flux tube for several solar rotations (i.e. on a time scale much longer than the classical emergence phase), or by torsional Alfvén waves.
Fil: Démoulin, Pascal. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia
Fil: Mandrini, Cristina Hemilse. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina
Fil: van Driel Gesztelyi, Lidia. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia
Fil: Thompson, B. J.. National Aeronautics and Space Administration. Goddart Institute for Space Studies; Estados Unidos
Fil: Plunkett, S.. Spece Sciences División. Naval Research Laboratory; Estados Unidos
Fil: Kovári, Zs.. Konkoly Observatory; Hungría
Fil: Aulanier, G.. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia
Fil: Young, A.. National Aeronautics and Space Administration. Goddart Institute for Space Studies; Estados Unidos
description An isolated active region (AR) was observed on the Sun during seven rotations, starting from its birth in July 1996 to its full dispersion in December 1996. We analyse the long-term budget of the AR relative magnetic helicity. Firstly, we calculate the helicity injected by differential rotation at the photospheric level using MDI/SoHO magnetograms. Secondly, we compute the coronal magnetic field and its helicity selecting the model which best fits the soft X-ray loops observed with SXT/Yohkoh. Finally, we identify all the coronal mass ejections (CMEs) that originated from the AR during its lifetime using LASCO and EIT/SoHO. Assuming a one to one correspondence between CMEs and magnetic clouds, we estimate the magnetic helicity which could be shed via CMEs. We find that differential rotation can neither provide the required magnetic helicity to the coronal field (at least a factor 2.5 to 4 larger), nor to the field ejected to the interplanetary space (a factor 4 to 20 larger), even in the case of this AR for which the total helicity injected by differential rotation is close to the maximum possible value. However, the total helicity ejected is equivalent to that of a twisted flux tube having the same magnetic flux as the studied AR and a number of turns in the interval [0.5,2.0]. We suggest that the main source of helicity is the inherent twist of the magnetic flux tube forming the active region. This magnetic helicity is transferred to the corona either by the continuous emergence of the flux tube for several solar rotations (i.e. on a time scale much longer than the classical emergence phase), or by torsional Alfvén waves.
publishDate 2002
dc.date.none.fl_str_mv 2002-02
dc.type.none.fl_str_mv info:eu-repo/semantics/article
info:eu-repo/semantics/publishedVersion
http://purl.org/coar/resource_type/c_6501
info:ar-repo/semantics/articulo
format article
status_str publishedVersion
dc.identifier.none.fl_str_mv http://hdl.handle.net/11336/22443
Démoulin, Pascal; Mandrini, Cristina Hemilse; van Driel Gesztelyi, Lidia; Thompson, B. J.; Plunkett, S.; et al.; What is the source of the magnetic helicity shed by CMEs? The long-term helicity budget of AR 7978; EDP Sciences; Astronomy and Astrophysics; 382; 2; 2-2002; 650-665
0004-6361
CONICET Digital
CONICET
url http://hdl.handle.net/11336/22443
identifier_str_mv Démoulin, Pascal; Mandrini, Cristina Hemilse; van Driel Gesztelyi, Lidia; Thompson, B. J.; Plunkett, S.; et al.; What is the source of the magnetic helicity shed by CMEs? The long-term helicity budget of AR 7978; EDP Sciences; Astronomy and Astrophysics; 382; 2; 2-2002; 650-665
0004-6361
CONICET Digital
CONICET
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361:20011634
info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/abs/2002/05/aa1962/aa1962.html
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
eu_rights_str_mv openAccess
rights_invalid_str_mv https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
dc.format.none.fl_str_mv application/pdf
application/pdf
dc.publisher.none.fl_str_mv EDP Sciences
publisher.none.fl_str_mv EDP Sciences
dc.source.none.fl_str_mv reponame:CONICET Digital (CONICET)
instname:Consejo Nacional de Investigaciones Científicas y Técnicas
reponame_str CONICET Digital (CONICET)
collection CONICET Digital (CONICET)
instname_str Consejo Nacional de Investigaciones Científicas y Técnicas
repository.name.fl_str_mv CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicas
repository.mail.fl_str_mv dasensio@conicet.gov.ar; lcarlino@conicet.gov.ar
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