Linking two consecutive non-merging magnetic clouds with their solar sources

Autores
Dasso, Sergio Ricardo; Mandrini, Cristina Hemilse; Schmieder, B.; Cremades, H.; Cid, C.; Cerrato, Y.; Saiz, E.; Démoulin, Pascal; Zhukov, A. N.; Rodriguez, L.; Aran, A.; Menvielle, M.; Poedts, S.
Año de publicación
2009
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
On 15 May 2005, a huge interplanetary coronal mass ejection (ICME) was observed near Earth. It triggered one of the most intense geomagnetic storms of solar cycle 23 (Dstpeak = −263 nT). This structure has been associated with the two-ribbon flare, filament eruption, and coronal mass ejection originating in active region 10759 (NOAA number). We analyze here the sequence of events, from solar wind measurements (at 1 AU) and back to the Sun, to understand the origin and evolution of this geoeffective ICME. From a detailed observational study of in situ magnetic field observations and plasma parameters in the interplanetary (IP) medium and the use of appropriate models we propose an alternative interpretation of the IP observations, different to those discussed in previous studies. In our view, the IP structure is formed by two extremely close consecutive magnetic clouds (MCs) that preserve their identity during their propagation through the interplanetary medium. Consequently, we identify two solar events in Hα and EUV which occurred in the source region of the MCs. The timing between solar and IP events, as well as the orientation of the MC axes and their associated solar arcades are in good agreement. Additionally, interplanetary radio type II observations allow the tracking of the multiple structures through inner heliosphere and pin down the interaction region to be located midway between the Sun and the Earth. The chain of observations from the photosphere to interplanetary space is in agreement with this scenario. Our analysis allows the detection of the solar sources of the transients and explains the extremely fast changes of the solar wind due to the transport of two attached (though nonmerging) MCs which affect the magnetosphere.
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: 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: Schmieder, B.. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia
Fil: Cremades, H.. Universidad Tecnológica Nacional; Argentina
Fil: Cid, C.. Universidad de Alcalá; España
Fil: Cerrato, Y.. Universidad de Alcalá; España
Fil: Saiz, E.. Universidad de Alcalá; España
Fil: Démoulin, Pascal. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia
Fil: Zhukov, A. N.. Royal Observatory of Belgium; Bélgica
Fil: Rodriguez, L.. Royal Observatory of Belgium; Bélgica
Fil: Aran, A.. Universidad de Barcelona; España
Fil: Menvielle, M.. Universite Paris Sud; Francia
Fil: Poedts, S.. Katholikie Universiteit Leuven; Bélgica
Materia
INTERPLANETARY PHYSICS: EJECTA, DRIVER GASES AND MAGNETIC CLOUDS
INTERPLANETARY PHYSICS: INTERPLANETARY MAGNETIC FIELDS
INTERPLANETARY PHYSICS: CORONAL MASS EJECTIONS
SOLAR PHYSICS: ASTROPHYSICS, AND ASTRONOMY: CORONAL MASS EJECTIONS
SOLAR PHYSICS: ASTROPHYSICS, AND ASTRONOMY: RADIO EMISSIONS
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:11336/24757
Acceder
id CONICETDig_8aa41b7e7ba648298a1556a964751ee0
oai_identifier_str oai:ri.conicet.gov.ar:11336/24757
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling Linking two consecutive non-merging magnetic clouds with their solar sourcesDasso, Sergio RicardoMandrini, Cristina HemilseSchmieder, B.Cremades, H.Cid, C.Cerrato, Y.Saiz, E.Démoulin, PascalZhukov, A. N.Rodriguez, L.Aran, A.Menvielle, M.Poedts, S.INTERPLANETARY PHYSICS: EJECTA, DRIVER GASES AND MAGNETIC CLOUDSINTERPLANETARY PHYSICS: INTERPLANETARY MAGNETIC FIELDSINTERPLANETARY PHYSICS: CORONAL MASS EJECTIONSSOLAR PHYSICS: ASTROPHYSICS, AND ASTRONOMY: CORONAL MASS EJECTIONSSOLAR PHYSICS: ASTROPHYSICS, AND ASTRONOMY: RADIO EMISSIONShttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1On 15 May 2005, a huge interplanetary coronal mass ejection (ICME) was observed near Earth. It triggered one of the most intense geomagnetic storms of solar cycle 23 (Dstpeak = −263 nT). This structure has been associated with the two-ribbon flare, filament eruption, and coronal mass ejection originating in active region 10759 (NOAA number). We analyze here the sequence of events, from solar wind measurements (at 1 AU) and back to the Sun, to understand the origin and evolution of this geoeffective ICME. From a detailed observational study of in situ magnetic field observations and plasma parameters in the interplanetary (IP) medium and the use of appropriate models we propose an alternative interpretation of the IP observations, different to those discussed in previous studies. In our view, the IP structure is formed by two extremely close consecutive magnetic clouds (MCs) that preserve their identity during their propagation through the interplanetary medium. Consequently, we identify two solar events in Hα and EUV which occurred in the source region of the MCs. The timing between solar and IP events, as well as the orientation of the MC axes and their associated solar arcades are in good agreement. Additionally, interplanetary radio type II observations allow the tracking of the multiple structures through inner heliosphere and pin down the interaction region to be located midway between the Sun and the Earth. The chain of observations from the photosphere to interplanetary space is in agreement with this scenario. Our analysis allows the detection of the solar sources of the transients and explains the extremely fast changes of the solar wind due to the transport of two attached (though nonmerging) MCs which affect the magnetosphere.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; ArgentinaFil: 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: Schmieder, B.. Centre National de la Recherche Scientifique. Observatoire de Paris; FranciaFil: Cremades, H.. Universidad Tecnológica Nacional; ArgentinaFil: Cid, C.. Universidad de Alcalá; EspañaFil: Cerrato, Y.. Universidad de Alcalá; EspañaFil: Saiz, E.. Universidad de Alcalá; EspañaFil: Démoulin, Pascal. Centre National de la Recherche Scientifique. Observatoire de Paris; FranciaFil: Zhukov, A. N.. Royal Observatory of Belgium; BélgicaFil: Rodriguez, L.. Royal Observatory of Belgium; BélgicaFil: Aran, A.. Universidad de Barcelona; EspañaFil: Menvielle, M.. Universite Paris Sud; FranciaFil: Poedts, S.. Katholikie Universiteit Leuven; BélgicaAmerican Geophysical Union2009-12info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/24757Dasso, Sergio Ricardo; Mandrini, Cristina Hemilse; Schmieder, B.; Cremades, H.; Cid, C.; et al.; Linking two consecutive non-merging magnetic clouds with their solar sources; American Geophysical Union; Journal of Geophysical Research; 114; A02109; 12-2009; 1-170148-0227CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1029/2008JA013102info:eu-repo/semantics/altIdentifier/url/http://onlinelibrary.wiley.com/doi/10.1029/2008JA013102/abstractinfo:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-03T09:56:01Zoai:ri.conicet.gov.ar:11336/24757instacron: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:34982025-09-03 09:56:01.922CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Linking two consecutive non-merging magnetic clouds with their solar sources
title Linking two consecutive non-merging magnetic clouds with their solar sources
spellingShingle Linking two consecutive non-merging magnetic clouds with their solar sources
Dasso, Sergio Ricardo
INTERPLANETARY PHYSICS: EJECTA, DRIVER GASES AND MAGNETIC CLOUDS
INTERPLANETARY PHYSICS: INTERPLANETARY MAGNETIC FIELDS
INTERPLANETARY PHYSICS: CORONAL MASS EJECTIONS
SOLAR PHYSICS: ASTROPHYSICS, AND ASTRONOMY: CORONAL MASS EJECTIONS
SOLAR PHYSICS: ASTROPHYSICS, AND ASTRONOMY: RADIO EMISSIONS
title_short Linking two consecutive non-merging magnetic clouds with their solar sources
title_full Linking two consecutive non-merging magnetic clouds with their solar sources
title_fullStr Linking two consecutive non-merging magnetic clouds with their solar sources
title_full_unstemmed Linking two consecutive non-merging magnetic clouds with their solar sources
title_sort Linking two consecutive non-merging magnetic clouds with their solar sources
dc.creator.none.fl_str_mv Dasso, Sergio Ricardo
Mandrini, Cristina Hemilse
Schmieder, B.
Cremades, H.
Cid, C.
Cerrato, Y.
Saiz, E.
Démoulin, Pascal
Zhukov, A. N.
Rodriguez, L.
Aran, A.
Menvielle, M.
Poedts, S.
author Dasso, Sergio Ricardo
author_facet Dasso, Sergio Ricardo
Mandrini, Cristina Hemilse
Schmieder, B.
Cremades, H.
Cid, C.
Cerrato, Y.
Saiz, E.
Démoulin, Pascal
Zhukov, A. N.
Rodriguez, L.
Aran, A.
Menvielle, M.
Poedts, S.
author_role author
author2 Mandrini, Cristina Hemilse
Schmieder, B.
Cremades, H.
Cid, C.
Cerrato, Y.
Saiz, E.
Démoulin, Pascal
Zhukov, A. N.
Rodriguez, L.
Aran, A.
Menvielle, M.
Poedts, S.
author2_role author
author
author
author
author
author
author
author
author
author
author
author
dc.subject.none.fl_str_mv INTERPLANETARY PHYSICS: EJECTA, DRIVER GASES AND MAGNETIC CLOUDS
INTERPLANETARY PHYSICS: INTERPLANETARY MAGNETIC FIELDS
INTERPLANETARY PHYSICS: CORONAL MASS EJECTIONS
SOLAR PHYSICS: ASTROPHYSICS, AND ASTRONOMY: CORONAL MASS EJECTIONS
SOLAR PHYSICS: ASTROPHYSICS, AND ASTRONOMY: RADIO EMISSIONS
topic INTERPLANETARY PHYSICS: EJECTA, DRIVER GASES AND MAGNETIC CLOUDS
INTERPLANETARY PHYSICS: INTERPLANETARY MAGNETIC FIELDS
INTERPLANETARY PHYSICS: CORONAL MASS EJECTIONS
SOLAR PHYSICS: ASTROPHYSICS, AND ASTRONOMY: CORONAL MASS EJECTIONS
SOLAR PHYSICS: ASTROPHYSICS, AND ASTRONOMY: RADIO EMISSIONS
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv On 15 May 2005, a huge interplanetary coronal mass ejection (ICME) was observed near Earth. It triggered one of the most intense geomagnetic storms of solar cycle 23 (Dstpeak = −263 nT). This structure has been associated with the two-ribbon flare, filament eruption, and coronal mass ejection originating in active region 10759 (NOAA number). We analyze here the sequence of events, from solar wind measurements (at 1 AU) and back to the Sun, to understand the origin and evolution of this geoeffective ICME. From a detailed observational study of in situ magnetic field observations and plasma parameters in the interplanetary (IP) medium and the use of appropriate models we propose an alternative interpretation of the IP observations, different to those discussed in previous studies. In our view, the IP structure is formed by two extremely close consecutive magnetic clouds (MCs) that preserve their identity during their propagation through the interplanetary medium. Consequently, we identify two solar events in Hα and EUV which occurred in the source region of the MCs. The timing between solar and IP events, as well as the orientation of the MC axes and their associated solar arcades are in good agreement. Additionally, interplanetary radio type II observations allow the tracking of the multiple structures through inner heliosphere and pin down the interaction region to be located midway between the Sun and the Earth. The chain of observations from the photosphere to interplanetary space is in agreement with this scenario. Our analysis allows the detection of the solar sources of the transients and explains the extremely fast changes of the solar wind due to the transport of two attached (though nonmerging) MCs which affect the magnetosphere.
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: 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: Schmieder, B.. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia
Fil: Cremades, H.. Universidad Tecnológica Nacional; Argentina
Fil: Cid, C.. Universidad de Alcalá; España
Fil: Cerrato, Y.. Universidad de Alcalá; España
Fil: Saiz, E.. Universidad de Alcalá; España
Fil: Démoulin, Pascal. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia
Fil: Zhukov, A. N.. Royal Observatory of Belgium; Bélgica
Fil: Rodriguez, L.. Royal Observatory of Belgium; Bélgica
Fil: Aran, A.. Universidad de Barcelona; España
Fil: Menvielle, M.. Universite Paris Sud; Francia
Fil: Poedts, S.. Katholikie Universiteit Leuven; Bélgica
description On 15 May 2005, a huge interplanetary coronal mass ejection (ICME) was observed near Earth. It triggered one of the most intense geomagnetic storms of solar cycle 23 (Dstpeak = −263 nT). This structure has been associated with the two-ribbon flare, filament eruption, and coronal mass ejection originating in active region 10759 (NOAA number). We analyze here the sequence of events, from solar wind measurements (at 1 AU) and back to the Sun, to understand the origin and evolution of this geoeffective ICME. From a detailed observational study of in situ magnetic field observations and plasma parameters in the interplanetary (IP) medium and the use of appropriate models we propose an alternative interpretation of the IP observations, different to those discussed in previous studies. In our view, the IP structure is formed by two extremely close consecutive magnetic clouds (MCs) that preserve their identity during their propagation through the interplanetary medium. Consequently, we identify two solar events in Hα and EUV which occurred in the source region of the MCs. The timing between solar and IP events, as well as the orientation of the MC axes and their associated solar arcades are in good agreement. Additionally, interplanetary radio type II observations allow the tracking of the multiple structures through inner heliosphere and pin down the interaction region to be located midway between the Sun and the Earth. The chain of observations from the photosphere to interplanetary space is in agreement with this scenario. Our analysis allows the detection of the solar sources of the transients and explains the extremely fast changes of the solar wind due to the transport of two attached (though nonmerging) MCs which affect the magnetosphere.
publishDate 2009
dc.date.none.fl_str_mv 2009-12
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/11336/24757
Dasso, Sergio Ricardo; Mandrini, Cristina Hemilse; Schmieder, B.; Cremades, H.; Cid, C.; et al.; Linking two consecutive non-merging magnetic clouds with their solar sources; American Geophysical Union; Journal of Geophysical Research; 114; A02109; 12-2009; 1-17
0148-0227
CONICET Digital
CONICET
url http://hdl.handle.net/11336/24757
identifier_str_mv Dasso, Sergio Ricardo; Mandrini, Cristina Hemilse; Schmieder, B.; Cremades, H.; Cid, C.; et al.; Linking two consecutive non-merging magnetic clouds with their solar sources; American Geophysical Union; Journal of Geophysical Research; 114; A02109; 12-2009; 1-17
0148-0227
CONICET Digital
CONICET
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/doi/10.1029/2008JA013102
info:eu-repo/semantics/altIdentifier/url/http://onlinelibrary.wiley.com/doi/10.1029/2008JA013102/abstract
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
application/pdf
dc.publisher.none.fl_str_mv American Geophysical Union
publisher.none.fl_str_mv American Geophysical Union
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 13.13397

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