Solar wind and IMF parameters associated with geomagnetic storms with Dst <- 50 nT

Autores
Mansilla, Gustavo Adolfo
Año de publicación
2008
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
A correlative study between the intensity of a geomagnetic storm (given by the Dst index) and the peak value reached by some solar wind parameters (velocity and density) and the southward component of the interplanetary magnetic field (IMF) is made. This study has been performed by using hourly values of the Dst index and measurements taken by the ACE spacecraft in the period 2000–2005, for which 72 geomagnetic storms were considered. It is confirmed that peak Dst is correlated to the maximum negative component Bz of the IMF better than the maxima of n and V (solar wind number density and speed, respectively). By considering all the storms, the correlation coefficient was found to be 0.88. If we consider the geomagnetic storms for which −200 nT < peak Dst < −60 nT, a lower correlation coefficient of 0.63 is obtained.
Fil: Mansilla, Gustavo Adolfo. Universidad Nacional de Tucumán. Facultad de Ciencias Exactas y Tecnología. Departamento de Física. Laboratorio de Ionósfera; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Tucumán; Argentina
Materia
Solar Wind
Geometric Storms
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:11336/81977
Acceder
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oai_identifier_str oai:ri.conicet.gov.ar:11336/81977
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling Solar wind and IMF parameters associated with geomagnetic storms with Dst <- 50 nTMansilla, Gustavo AdolfoSolar WindGeometric Stormshttps://purl.org/becyt/ford/1.5https://purl.org/becyt/ford/1A correlative study between the intensity of a geomagnetic storm (given by the Dst index) and the peak value reached by some solar wind parameters (velocity and density) and the southward component of the interplanetary magnetic field (IMF) is made. This study has been performed by using hourly values of the Dst index and measurements taken by the ACE spacecraft in the period 2000–2005, for which 72 geomagnetic storms were considered. It is confirmed that peak Dst is correlated to the maximum negative component Bz of the IMF better than the maxima of n and V (solar wind number density and speed, respectively). By considering all the storms, the correlation coefficient was found to be 0.88. If we consider the geomagnetic storms for which −200 nT < peak Dst < −60 nT, a lower correlation coefficient of 0.63 is obtained.Fil: Mansilla, Gustavo Adolfo. Universidad Nacional de Tucumán. Facultad de Ciencias Exactas y Tecnología. Departamento de Física. Laboratorio de Ionósfera; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Tucumán; ArgentinaIOP Publishing on behalf of the Royal Swedish Academy of Sciences2008-12info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/81977Mansilla, Gustavo Adolfo; Solar wind and IMF parameters associated with geomagnetic storms with Dst <- 50 nT; IOP Publishing on behalf of the Royal Swedish Academy of Sciences; PHYSICA SCRIPTA; 78; 12-2008; 1-40031-8949CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1088/0031-8949/78/04/045902info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T09:59:46Zoai:ri.conicet.gov.ar:11336/81977instacron: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 09:59:47.082CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Solar wind and IMF parameters associated with geomagnetic storms with Dst <- 50 nT
title Solar wind and IMF parameters associated with geomagnetic storms with Dst <- 50 nT
spellingShingle Solar wind and IMF parameters associated with geomagnetic storms with Dst <- 50 nT
Mansilla, Gustavo Adolfo
Solar Wind
Geometric Storms
title_short Solar wind and IMF parameters associated with geomagnetic storms with Dst <- 50 nT
title_full Solar wind and IMF parameters associated with geomagnetic storms with Dst <- 50 nT
title_fullStr Solar wind and IMF parameters associated with geomagnetic storms with Dst <- 50 nT
title_full_unstemmed Solar wind and IMF parameters associated with geomagnetic storms with Dst <- 50 nT
title_sort Solar wind and IMF parameters associated with geomagnetic storms with Dst <- 50 nT
dc.creator.none.fl_str_mv Mansilla, Gustavo Adolfo
author Mansilla, Gustavo Adolfo
author_facet Mansilla, Gustavo Adolfo
author_role author
dc.subject.none.fl_str_mv Solar Wind
Geometric Storms
topic Solar Wind
Geometric Storms
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.5
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv A correlative study between the intensity of a geomagnetic storm (given by the Dst index) and the peak value reached by some solar wind parameters (velocity and density) and the southward component of the interplanetary magnetic field (IMF) is made. This study has been performed by using hourly values of the Dst index and measurements taken by the ACE spacecraft in the period 2000–2005, for which 72 geomagnetic storms were considered. It is confirmed that peak Dst is correlated to the maximum negative component Bz of the IMF better than the maxima of n and V (solar wind number density and speed, respectively). By considering all the storms, the correlation coefficient was found to be 0.88. If we consider the geomagnetic storms for which −200 nT < peak Dst < −60 nT, a lower correlation coefficient of 0.63 is obtained.
Fil: Mansilla, Gustavo Adolfo. Universidad Nacional de Tucumán. Facultad de Ciencias Exactas y Tecnología. Departamento de Física. Laboratorio de Ionósfera; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Tucumán; Argentina
description A correlative study between the intensity of a geomagnetic storm (given by the Dst index) and the peak value reached by some solar wind parameters (velocity and density) and the southward component of the interplanetary magnetic field (IMF) is made. This study has been performed by using hourly values of the Dst index and measurements taken by the ACE spacecraft in the period 2000–2005, for which 72 geomagnetic storms were considered. It is confirmed that peak Dst is correlated to the maximum negative component Bz of the IMF better than the maxima of n and V (solar wind number density and speed, respectively). By considering all the storms, the correlation coefficient was found to be 0.88. If we consider the geomagnetic storms for which −200 nT < peak Dst < −60 nT, a lower correlation coefficient of 0.63 is obtained.
publishDate 2008
dc.date.none.fl_str_mv 2008-12
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/11336/81977
Mansilla, Gustavo Adolfo; Solar wind and IMF parameters associated with geomagnetic storms with Dst <- 50 nT; IOP Publishing on behalf of the Royal Swedish Academy of Sciences; PHYSICA SCRIPTA; 78; 12-2008; 1-4
0031-8949
CONICET Digital
CONICET
url http://hdl.handle.net/11336/81977
identifier_str_mv Mansilla, Gustavo Adolfo; Solar wind and IMF parameters associated with geomagnetic storms with Dst <- 50 nT; IOP Publishing on behalf of the Royal Swedish Academy of Sciences; PHYSICA SCRIPTA; 78; 12-2008; 1-4
0031-8949
CONICET Digital
CONICET
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/doi/10.1088/0031-8949/78/04/045902
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 IOP Publishing on behalf of the Royal Swedish Academy of Sciences
publisher.none.fl_str_mv IOP Publishing on behalf of the Royal Swedish Academy of 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
_version_ 1844613771838881792
score 13.070432

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