Typical Profiles and Distributions of Plasma and Magnetic Field Parameters in Magnetic Clouds at 1 AU
- Autores
- Rodriguez, L.; Masías Meza, Jimmy Joel; Dasso, Sergio Ricardo; Démoulin, Pascal; Zhukov, A. N.; Gulisano, Adriana Maria; Mierla, M.; Kilpua, E.; West, M.; Lacatus, D.; Paraschiv, A.; Janvier, M.
- Año de publicación
- 2016
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- Magnetic clouds (MCs) are a subset of interplanetary coronal mass ejections (ICMEs). They are important because of their simple internal magnetic field configuration, which resembles a magnetic flux rope, and because they represent one of the most geoeffective types of solar transients. In this study, we analyze their internal structure using a superposed epoch method on 63 events observed at L1 by the Advance Composition Explorer (ACE), between 1998 and 2006. In this way, we obtain an average profile for each plasma and magnetic field parameter at each point of the cloud. Furthermore, we take a fixed time-window upstream and downstream from the MC to also sample the regions preceding the cloud and the wake trailing it. We then perform a detailed analysis of the internal characteristics of the clouds and their surrounding solar wind environments. We find that the parameters studied are compatible with log-normal distribution functions. The plasma β and the level of fluctuations in the magnetic field vector are the best parameters to define the boundaries of MCs. We find that one third of the events shows a peak in plasma density close to the trailing edge of the flux ropes. We provide several possible explanations for this result and investigate if the density peak is of a solar origin (e.g. erupting prominence material) or formed during the magnetic cloud travel from the Sun to 1 AU. The most plausible explanation is the compression due to a fast overtaking flow, coming from a coronal hole located to the east of the solar source region of the magnetic cloud.
Fil: Rodriguez, L.. Royal Observatory Of Belgium; ; Bélgica
Fil: Masías Meza, Jimmy Joel. Consejo Nacional de Investigaciones Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Física de Buenos Aires. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Física de Buenos Aires; 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: Démoulin, Pascal. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia
Fil: Zhukov, A. N.. Royal Observatory Of Belgium; Bélgica
Fil: Gulisano, Adriana Maria. Ministerio de Relaciones Exteriores, Comercio Interno y Culto. Dirección Nacional del Antártico. Instituto Antártico Argentino; Argentina
Fil: Mierla, M.. Royal Observatory Of Belgium; Bélgica
Fil: Kilpua, E.. Helsingin Yliopisto; ; Finlandia
Fil: West, M.. Royal Observatory Of Belgium; ; Bélgica
Fil: Lacatus, D.. Monash University; Australia
Fil: Paraschiv, A.. Monash University; Australia
Fil: Janvier, M.. Universite Paris-sud Xi;; Francia - Materia
-
CORONAL MASS EJECTIONS, LOW CORONAL SIGNATURES, INITIATION AND PROPAGATION
INTERPLANETARY CORONAL MASS EJECTIONS
MAGNETIC CLOUDS
SPACE WEATHER - 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:11336/85698
Ver los metadatos del registro completo
id |
CONICETDig_21c6b6c1fff0a465a331fbc76f0256b4 |
---|---|
oai_identifier_str |
oai:ri.conicet.gov.ar:11336/85698 |
network_acronym_str |
CONICETDig |
repository_id_str |
3498 |
network_name_str |
CONICET Digital (CONICET) |
spelling |
Typical Profiles and Distributions of Plasma and Magnetic Field Parameters in Magnetic Clouds at 1 AURodriguez, L.Masías Meza, Jimmy JoelDasso, Sergio RicardoDémoulin, PascalZhukov, A. N.Gulisano, Adriana MariaMierla, M.Kilpua, E.West, M.Lacatus, D.Paraschiv, A.Janvier, M.CORONAL MASS EJECTIONS, LOW CORONAL SIGNATURES, INITIATION AND PROPAGATIONINTERPLANETARY CORONAL MASS EJECTIONSMAGNETIC CLOUDSSPACE WEATHERhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Magnetic clouds (MCs) are a subset of interplanetary coronal mass ejections (ICMEs). They are important because of their simple internal magnetic field configuration, which resembles a magnetic flux rope, and because they represent one of the most geoeffective types of solar transients. In this study, we analyze their internal structure using a superposed epoch method on 63 events observed at L1 by the Advance Composition Explorer (ACE), between 1998 and 2006. In this way, we obtain an average profile for each plasma and magnetic field parameter at each point of the cloud. Furthermore, we take a fixed time-window upstream and downstream from the MC to also sample the regions preceding the cloud and the wake trailing it. We then perform a detailed analysis of the internal characteristics of the clouds and their surrounding solar wind environments. We find that the parameters studied are compatible with log-normal distribution functions. The plasma β and the level of fluctuations in the magnetic field vector are the best parameters to define the boundaries of MCs. We find that one third of the events shows a peak in plasma density close to the trailing edge of the flux ropes. We provide several possible explanations for this result and investigate if the density peak is of a solar origin (e.g. erupting prominence material) or formed during the magnetic cloud travel from the Sun to 1 AU. The most plausible explanation is the compression due to a fast overtaking flow, coming from a coronal hole located to the east of the solar source region of the magnetic cloud.Fil: Rodriguez, L.. Royal Observatory Of Belgium; ; BélgicaFil: Masías Meza, Jimmy Joel. Consejo Nacional de Investigaciones Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Física de Buenos Aires. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Física de Buenos Aires; 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: Démoulin, Pascal. Centre National de la Recherche Scientifique. Observatoire de Paris; FranciaFil: Zhukov, A. N.. Royal Observatory Of Belgium; BélgicaFil: Gulisano, Adriana Maria. Ministerio de Relaciones Exteriores, Comercio Interno y Culto. Dirección Nacional del Antártico. Instituto Antártico Argentino; ArgentinaFil: Mierla, M.. Royal Observatory Of Belgium; BélgicaFil: Kilpua, E.. Helsingin Yliopisto; ; FinlandiaFil: West, M.. Royal Observatory Of Belgium; ; BélgicaFil: Lacatus, D.. Monash University; AustraliaFil: Paraschiv, A.. Monash University; AustraliaFil: Janvier, M.. Universite Paris-sud Xi;; FranciaSpringer2016-07info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/85698Rodriguez, L.; Masías Meza, Jimmy Joel; Dasso, Sergio Ricardo; Démoulin, Pascal; Zhukov, A. N.; et al.; Typical Profiles and Distributions of Plasma and Magnetic Field Parameters in Magnetic Clouds at 1 AU; Springer; Solar Physics; 291; 7; 7-2016; 2145-21630038-0938CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1007/s11207-016-0955-5info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-10-22T11:11:27Zoai:ri.conicet.gov.ar:11336/85698instacron: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:34982025-10-22 11:11:27.707CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse |
dc.title.none.fl_str_mv |
Typical Profiles and Distributions of Plasma and Magnetic Field Parameters in Magnetic Clouds at 1 AU |
title |
Typical Profiles and Distributions of Plasma and Magnetic Field Parameters in Magnetic Clouds at 1 AU |
spellingShingle |
Typical Profiles and Distributions of Plasma and Magnetic Field Parameters in Magnetic Clouds at 1 AU Rodriguez, L. CORONAL MASS EJECTIONS, LOW CORONAL SIGNATURES, INITIATION AND PROPAGATION INTERPLANETARY CORONAL MASS EJECTIONS MAGNETIC CLOUDS SPACE WEATHER |
title_short |
Typical Profiles and Distributions of Plasma and Magnetic Field Parameters in Magnetic Clouds at 1 AU |
title_full |
Typical Profiles and Distributions of Plasma and Magnetic Field Parameters in Magnetic Clouds at 1 AU |
title_fullStr |
Typical Profiles and Distributions of Plasma and Magnetic Field Parameters in Magnetic Clouds at 1 AU |
title_full_unstemmed |
Typical Profiles and Distributions of Plasma and Magnetic Field Parameters in Magnetic Clouds at 1 AU |
title_sort |
Typical Profiles and Distributions of Plasma and Magnetic Field Parameters in Magnetic Clouds at 1 AU |
dc.creator.none.fl_str_mv |
Rodriguez, L. Masías Meza, Jimmy Joel Dasso, Sergio Ricardo Démoulin, Pascal Zhukov, A. N. Gulisano, Adriana Maria Mierla, M. Kilpua, E. West, M. Lacatus, D. Paraschiv, A. Janvier, M. |
author |
Rodriguez, L. |
author_facet |
Rodriguez, L. Masías Meza, Jimmy Joel Dasso, Sergio Ricardo Démoulin, Pascal Zhukov, A. N. Gulisano, Adriana Maria Mierla, M. Kilpua, E. West, M. Lacatus, D. Paraschiv, A. Janvier, M. |
author_role |
author |
author2 |
Masías Meza, Jimmy Joel Dasso, Sergio Ricardo Démoulin, Pascal Zhukov, A. N. Gulisano, Adriana Maria Mierla, M. Kilpua, E. West, M. Lacatus, D. Paraschiv, A. Janvier, M. |
author2_role |
author author author author author author author author author author author |
dc.subject.none.fl_str_mv |
CORONAL MASS EJECTIONS, LOW CORONAL SIGNATURES, INITIATION AND PROPAGATION INTERPLANETARY CORONAL MASS EJECTIONS MAGNETIC CLOUDS SPACE WEATHER |
topic |
CORONAL MASS EJECTIONS, LOW CORONAL SIGNATURES, INITIATION AND PROPAGATION INTERPLANETARY CORONAL MASS EJECTIONS MAGNETIC CLOUDS SPACE WEATHER |
purl_subject.fl_str_mv |
https://purl.org/becyt/ford/1.3 https://purl.org/becyt/ford/1 |
dc.description.none.fl_txt_mv |
Magnetic clouds (MCs) are a subset of interplanetary coronal mass ejections (ICMEs). They are important because of their simple internal magnetic field configuration, which resembles a magnetic flux rope, and because they represent one of the most geoeffective types of solar transients. In this study, we analyze their internal structure using a superposed epoch method on 63 events observed at L1 by the Advance Composition Explorer (ACE), between 1998 and 2006. In this way, we obtain an average profile for each plasma and magnetic field parameter at each point of the cloud. Furthermore, we take a fixed time-window upstream and downstream from the MC to also sample the regions preceding the cloud and the wake trailing it. We then perform a detailed analysis of the internal characteristics of the clouds and their surrounding solar wind environments. We find that the parameters studied are compatible with log-normal distribution functions. The plasma β and the level of fluctuations in the magnetic field vector are the best parameters to define the boundaries of MCs. We find that one third of the events shows a peak in plasma density close to the trailing edge of the flux ropes. We provide several possible explanations for this result and investigate if the density peak is of a solar origin (e.g. erupting prominence material) or formed during the magnetic cloud travel from the Sun to 1 AU. The most plausible explanation is the compression due to a fast overtaking flow, coming from a coronal hole located to the east of the solar source region of the magnetic cloud. Fil: Rodriguez, L.. Royal Observatory Of Belgium; ; Bélgica Fil: Masías Meza, Jimmy Joel. Consejo Nacional de Investigaciones Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Física de Buenos Aires. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Física de Buenos Aires; 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: Démoulin, Pascal. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia Fil: Zhukov, A. N.. Royal Observatory Of Belgium; Bélgica Fil: Gulisano, Adriana Maria. Ministerio de Relaciones Exteriores, Comercio Interno y Culto. Dirección Nacional del Antártico. Instituto Antártico Argentino; Argentina Fil: Mierla, M.. Royal Observatory Of Belgium; Bélgica Fil: Kilpua, E.. Helsingin Yliopisto; ; Finlandia Fil: West, M.. Royal Observatory Of Belgium; ; Bélgica Fil: Lacatus, D.. Monash University; Australia Fil: Paraschiv, A.. Monash University; Australia Fil: Janvier, M.. Universite Paris-sud Xi;; Francia |
description |
Magnetic clouds (MCs) are a subset of interplanetary coronal mass ejections (ICMEs). They are important because of their simple internal magnetic field configuration, which resembles a magnetic flux rope, and because they represent one of the most geoeffective types of solar transients. In this study, we analyze their internal structure using a superposed epoch method on 63 events observed at L1 by the Advance Composition Explorer (ACE), between 1998 and 2006. In this way, we obtain an average profile for each plasma and magnetic field parameter at each point of the cloud. Furthermore, we take a fixed time-window upstream and downstream from the MC to also sample the regions preceding the cloud and the wake trailing it. We then perform a detailed analysis of the internal characteristics of the clouds and their surrounding solar wind environments. We find that the parameters studied are compatible with log-normal distribution functions. The plasma β and the level of fluctuations in the magnetic field vector are the best parameters to define the boundaries of MCs. We find that one third of the events shows a peak in plasma density close to the trailing edge of the flux ropes. We provide several possible explanations for this result and investigate if the density peak is of a solar origin (e.g. erupting prominence material) or formed during the magnetic cloud travel from the Sun to 1 AU. The most plausible explanation is the compression due to a fast overtaking flow, coming from a coronal hole located to the east of the solar source region of the magnetic cloud. |
publishDate |
2016 |
dc.date.none.fl_str_mv |
2016-07 |
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/11336/85698 Rodriguez, L.; Masías Meza, Jimmy Joel; Dasso, Sergio Ricardo; Démoulin, Pascal; Zhukov, A. N.; et al.; Typical Profiles and Distributions of Plasma and Magnetic Field Parameters in Magnetic Clouds at 1 AU; Springer; Solar Physics; 291; 7; 7-2016; 2145-2163 0038-0938 CONICET Digital CONICET |
url |
http://hdl.handle.net/11336/85698 |
identifier_str_mv |
Rodriguez, L.; Masías Meza, Jimmy Joel; Dasso, Sergio Ricardo; Démoulin, Pascal; Zhukov, A. N.; et al.; Typical Profiles and Distributions of Plasma and Magnetic Field Parameters in Magnetic Clouds at 1 AU; Springer; Solar Physics; 291; 7; 7-2016; 2145-2163 0038-0938 CONICET Digital CONICET |
dc.language.none.fl_str_mv |
eng |
language |
eng |
dc.relation.none.fl_str_mv |
info:eu-repo/semantics/altIdentifier/doi/10.1007/s11207-016-0955-5 |
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 |
Springer |
publisher.none.fl_str_mv |
Springer |
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 |
_version_ |
1846781492524482560 |
score |
12.982451 |