Actors of the main activity in large complex centres during the 23 solar cycle maximum

Autores
Schmieder, B.; Démoulin, Pascal; Pariat, E.; Török, T.; Molodij, G.; Mandrini, Cristina Hemilse; Dasso, Sergio Ricardo; Chandra, R.; Uddin, W.; Kumar, P.; Manoharan, P.K.; Venkatakrishnan, P.; Srivastava, N.
Año de publicación
2011
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
During the maximum of Solar Cycle 23, large active regions had a long life, spanning several solar rotations, and produced large numbers of X-class flares and CMEs, some of them associated to magnetic clouds (MCs). This is the case for the Halloween active regions in 2003. The most geoeffective MC of the cycle (Dst = 457) had its source during the disk passage of one of these active regions (NOAA 10501) on 18 November 2003. Such an activity was presumably due to continuous emerging magnetic flux that was observed during this passage. Moreover, the region exhibited a complex topology with multiple domains of different magnetic helicities. The complexity was observed to reach such unprecedented levels that a detailed multi-wavelength analysis is necessary to precisely identify the solar sources of CMEs and MCs. Magnetic clouds are identified using in situ measurements and interplanetary scintillation (IPS) data. Results from these two different sets of data are also compared.
Fil: Schmieder, B.. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia
Fil: Démoulin, Pascal. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia
Fil: Pariat, E.. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia
Fil: Török, T.. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia
Fil: Molodij, G.. 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: Dasso, Sergio Ricardo. 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: Chandra, R.. Kumaun University; India
Fil: Uddin, W.. ARIES; India
Fil: Kumar, P.. ARIES; India
Fil: Manoharan, P.K.. Tata Institute of Fundamental research,; India
Fil: Venkatakrishnan, P.. Udaipur Solar Observatory; India
Fil: Srivastava, N.. Udaipur Solar Observatory; India
Materia
Solar Flares
Coronal Mass Ejections
Magnetic Clouds
Interplanetary Scintillation
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:11336/19638
Acceder
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oai_identifier_str oai:ri.conicet.gov.ar:11336/19638
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling Actors of the main activity in large complex centres during the 23 solar cycle maximumSchmieder, B.Démoulin, PascalPariat, E.Török, T.Molodij, G.Mandrini, Cristina HemilseDasso, Sergio RicardoChandra, R.Uddin, W.Kumar, P.Manoharan, P.K.Venkatakrishnan, P.Srivastava, N.Solar FlaresCoronal Mass EjectionsMagnetic CloudsInterplanetary Scintillationhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1During the maximum of Solar Cycle 23, large active regions had a long life, spanning several solar rotations, and produced large numbers of X-class flares and CMEs, some of them associated to magnetic clouds (MCs). This is the case for the Halloween active regions in 2003. The most geoeffective MC of the cycle (Dst = 457) had its source during the disk passage of one of these active regions (NOAA 10501) on 18 November 2003. Such an activity was presumably due to continuous emerging magnetic flux that was observed during this passage. Moreover, the region exhibited a complex topology with multiple domains of different magnetic helicities. The complexity was observed to reach such unprecedented levels that a detailed multi-wavelength analysis is necessary to precisely identify the solar sources of CMEs and MCs. Magnetic clouds are identified using in situ measurements and interplanetary scintillation (IPS) data. Results from these two different sets of data are also compared.Fil: Schmieder, B.. Centre National de la Recherche Scientifique. Observatoire de Paris; FranciaFil: Démoulin, Pascal. Centre National de la Recherche Scientifique. Observatoire de Paris; FranciaFil: Pariat, E.. Centre National de la Recherche Scientifique. Observatoire de Paris; FranciaFil: Török, T.. Centre National de la Recherche Scientifique. Observatoire de Paris; FranciaFil: Molodij, G.. 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: Dasso, Sergio Ricardo. 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: Chandra, R.. Kumaun University; IndiaFil: Uddin, W.. ARIES; IndiaFil: Kumar, P.. ARIES; IndiaFil: Manoharan, P.K.. Tata Institute of Fundamental research,; IndiaFil: Venkatakrishnan, P.. Udaipur Solar Observatory; IndiaFil: Srivastava, N.. Udaipur Solar Observatory; IndiaElsevier2011-02info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/19638Schmieder, B.; Démoulin, Pascal; Pariat, E.; Török, T.; Molodij, G.; et al.; Actors of the main activity in large complex centres during the 23 solar cycle maximum; Elsevier; Advances in Space Research; 47; 12; 2-2011; 2081-20910273-1177CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1016/j.asr.2011.02.001info:eu-repo/semantics/altIdentifier/url/http://www.sciencedirect.com/science/article/pii/S0273117711000937info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-10T13:03:11Zoai:ri.conicet.gov.ar:11336/19638instacron: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:34982025-09-10 13:03:11.39CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Actors of the main activity in large complex centres during the 23 solar cycle maximum
title Actors of the main activity in large complex centres during the 23 solar cycle maximum
spellingShingle Actors of the main activity in large complex centres during the 23 solar cycle maximum
Schmieder, B.
Solar Flares
Coronal Mass Ejections
Magnetic Clouds
Interplanetary Scintillation
title_short Actors of the main activity in large complex centres during the 23 solar cycle maximum
title_full Actors of the main activity in large complex centres during the 23 solar cycle maximum
title_fullStr Actors of the main activity in large complex centres during the 23 solar cycle maximum
title_full_unstemmed Actors of the main activity in large complex centres during the 23 solar cycle maximum
title_sort Actors of the main activity in large complex centres during the 23 solar cycle maximum
dc.creator.none.fl_str_mv Schmieder, B.
Démoulin, Pascal
Pariat, E.
Török, T.
Molodij, G.
Mandrini, Cristina Hemilse
Dasso, Sergio Ricardo
Chandra, R.
Uddin, W.
Kumar, P.
Manoharan, P.K.
Venkatakrishnan, P.
Srivastava, N.
author Schmieder, B.
author_facet Schmieder, B.
Démoulin, Pascal
Pariat, E.
Török, T.
Molodij, G.
Mandrini, Cristina Hemilse
Dasso, Sergio Ricardo
Chandra, R.
Uddin, W.
Kumar, P.
Manoharan, P.K.
Venkatakrishnan, P.
Srivastava, N.
author_role author
author2 Démoulin, Pascal
Pariat, E.
Török, T.
Molodij, G.
Mandrini, Cristina Hemilse
Dasso, Sergio Ricardo
Chandra, R.
Uddin, W.
Kumar, P.
Manoharan, P.K.
Venkatakrishnan, P.
Srivastava, N.
author2_role author
author
author
author
author
author
author
author
author
author
author
author
dc.subject.none.fl_str_mv Solar Flares
Coronal Mass Ejections
Magnetic Clouds
Interplanetary Scintillation
topic Solar Flares
Coronal Mass Ejections
Magnetic Clouds
Interplanetary Scintillation
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv During the maximum of Solar Cycle 23, large active regions had a long life, spanning several solar rotations, and produced large numbers of X-class flares and CMEs, some of them associated to magnetic clouds (MCs). This is the case for the Halloween active regions in 2003. The most geoeffective MC of the cycle (Dst = 457) had its source during the disk passage of one of these active regions (NOAA 10501) on 18 November 2003. Such an activity was presumably due to continuous emerging magnetic flux that was observed during this passage. Moreover, the region exhibited a complex topology with multiple domains of different magnetic helicities. The complexity was observed to reach such unprecedented levels that a detailed multi-wavelength analysis is necessary to precisely identify the solar sources of CMEs and MCs. Magnetic clouds are identified using in situ measurements and interplanetary scintillation (IPS) data. Results from these two different sets of data are also compared.
Fil: Schmieder, B.. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia
Fil: Démoulin, Pascal. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia
Fil: Pariat, E.. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia
Fil: Török, T.. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia
Fil: Molodij, G.. 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: Dasso, Sergio Ricardo. 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: Chandra, R.. Kumaun University; India
Fil: Uddin, W.. ARIES; India
Fil: Kumar, P.. ARIES; India
Fil: Manoharan, P.K.. Tata Institute of Fundamental research,; India
Fil: Venkatakrishnan, P.. Udaipur Solar Observatory; India
Fil: Srivastava, N.. Udaipur Solar Observatory; India
description During the maximum of Solar Cycle 23, large active regions had a long life, spanning several solar rotations, and produced large numbers of X-class flares and CMEs, some of them associated to magnetic clouds (MCs). This is the case for the Halloween active regions in 2003. The most geoeffective MC of the cycle (Dst = 457) had its source during the disk passage of one of these active regions (NOAA 10501) on 18 November 2003. Such an activity was presumably due to continuous emerging magnetic flux that was observed during this passage. Moreover, the region exhibited a complex topology with multiple domains of different magnetic helicities. The complexity was observed to reach such unprecedented levels that a detailed multi-wavelength analysis is necessary to precisely identify the solar sources of CMEs and MCs. Magnetic clouds are identified using in situ measurements and interplanetary scintillation (IPS) data. Results from these two different sets of data are also compared.
publishDate 2011
dc.date.none.fl_str_mv 2011-02
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/11336/19638
Schmieder, B.; Démoulin, Pascal; Pariat, E.; Török, T.; Molodij, G.; et al.; Actors of the main activity in large complex centres during the 23 solar cycle maximum; Elsevier; Advances in Space Research; 47; 12; 2-2011; 2081-2091
0273-1177
CONICET Digital
CONICET
url http://hdl.handle.net/11336/19638
identifier_str_mv Schmieder, B.; Démoulin, Pascal; Pariat, E.; Török, T.; Molodij, G.; et al.; Actors of the main activity in large complex centres during the 23 solar cycle maximum; Elsevier; Advances in Space Research; 47; 12; 2-2011; 2081-2091
0273-1177
CONICET Digital
CONICET
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/doi/10.1016/j.asr.2011.02.001
info:eu-repo/semantics/altIdentifier/url/http://www.sciencedirect.com/science/article/pii/S0273117711000937
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
application/pdf
dc.publisher.none.fl_str_mv Elsevier
publisher.none.fl_str_mv Elsevier
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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score 12.993085

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