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
- Institución
- Consejo Nacional de Investigaciones Científicas y Técnicas
- OAI Identificador
- oai:ri.conicet.gov.ar:11336/22443
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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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1844613760004653056 |
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13.070432 |