The geomagnetic solar flare effect identified by SIIG as an indicator of a solar flare observed by GOES satellites

Autores
Van Zele, Maria Andrea; Meza, A.
Año de publicación
2011
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
This paper studies the efficiency of geomagnetic solar flare effects (gsfe) in X solar flare detection; so during the period 1999?2007 a comparison between solar flare (sf) observed by satellites of the Geostationary Operational Environmental Satellite (GOES) programme and gsfe published by the Service International des Indices Geomagnetiques (SIIG) is made.Solar flares (sfs) are one of the most powerful manifestations of the solar activity. Because the far UV and soft and hard X-ray solar flare radiation is absorbed by the ionosphere, the ionized gas density increases (ionospheric solar flare effect, isfe) and a sudden enhancement of geomagnetic field near Earth surface (geomagnetic solar flare effect, gsfe) is produced.The solar X-ray flux is systematically recorded since 1975 by GOES satellites, and gsfe are declared by geomagnetic observatories since 1957. We corroborate that the identification of sf using gsfe is affected by several factors:? the intensity and average growth rate of solar flare radiation when quicker is it more easily the sf is detected as gsfe;? the position of the geomagnetic observatory, we found that observatories placed at summer hemisphere identify more easily the sf, sothe uneven geographical distribution of observatories make the sf identification difficult;? the existing geomagnetic perturbation previous to sf, and the likeness between the gsfe and other geomagnetic variations.This work shows that gsfe recorded as associated to sf is a poor detector of sf even if it is intense. Some of these inconveniences can be avoided if the distribution of the observatories is improved and the identification of a sf is made using simultaneously gsfe, solar wind parameters and isfe.
Fil: Van Zele, Maria Andrea. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Departamento de Geología; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Geociencias Básicas, Aplicadas y Ambientales de Buenos Aires. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Geociencias Básicas, Aplicadas y Ambientales de Buenos Aires; Argentina
Fil: Meza, A.. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina
Materia
Solar flare effect
Geomagnetic field
GPS
Total electron content
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:11336/280060
Acceder
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network_name_str CONICET Digital (CONICET)
spelling The geomagnetic solar flare effect identified by SIIG as an indicator of a solar flare observed by GOES satellitesVan Zele, Maria AndreaMeza, A.Solar flare effectGeomagnetic fieldGPSTotal electron contenthttps://purl.org/becyt/ford/1.5https://purl.org/becyt/ford/1This paper studies the efficiency of geomagnetic solar flare effects (gsfe) in X solar flare detection; so during the period 1999?2007 a comparison between solar flare (sf) observed by satellites of the Geostationary Operational Environmental Satellite (GOES) programme and gsfe published by the Service International des Indices Geomagnetiques (SIIG) is made.Solar flares (sfs) are one of the most powerful manifestations of the solar activity. Because the far UV and soft and hard X-ray solar flare radiation is absorbed by the ionosphere, the ionized gas density increases (ionospheric solar flare effect, isfe) and a sudden enhancement of geomagnetic field near Earth surface (geomagnetic solar flare effect, gsfe) is produced.The solar X-ray flux is systematically recorded since 1975 by GOES satellites, and gsfe are declared by geomagnetic observatories since 1957. We corroborate that the identification of sf using gsfe is affected by several factors:? the intensity and average growth rate of solar flare radiation when quicker is it more easily the sf is detected as gsfe;? the position of the geomagnetic observatory, we found that observatories placed at summer hemisphere identify more easily the sf, sothe uneven geographical distribution of observatories make the sf identification difficult;? the existing geomagnetic perturbation previous to sf, and the likeness between the gsfe and other geomagnetic variations.This work shows that gsfe recorded as associated to sf is a poor detector of sf even if it is intense. Some of these inconveniences can be avoided if the distribution of the observatories is improved and the identification of a sf is made using simultaneously gsfe, solar wind parameters and isfe.Fil: Van Zele, Maria Andrea. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Departamento de Geología; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Geociencias Básicas, Aplicadas y Ambientales de Buenos Aires. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Geociencias Básicas, Aplicadas y Ambientales de Buenos Aires; ArgentinaFil: Meza, A.. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; ArgentinaElsevier2011-09info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/280060Van Zele, Maria Andrea; Meza, A.; The geomagnetic solar flare effect identified by SIIG as an indicator of a solar flare observed by GOES satellites; Elsevier; Advances in Space Research; 48; 5; 9-2011; 826-8360273-1177CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://www.sciencedirect.com/science/article/abs/pii/S0273117711003103info:eu-repo/semantics/altIdentifier/doi/10.1016/j.asr.2011.04.037info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2026-02-06T12:42:05Zoai:ri.conicet.gov.ar:11336/280060instacron: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:34982026-02-06 12:42:05.435CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv The geomagnetic solar flare effect identified by SIIG as an indicator of a solar flare observed by GOES satellites
title The geomagnetic solar flare effect identified by SIIG as an indicator of a solar flare observed by GOES satellites
spellingShingle The geomagnetic solar flare effect identified by SIIG as an indicator of a solar flare observed by GOES satellites
Van Zele, Maria Andrea
Solar flare effect
Geomagnetic field
GPS
Total electron content
title_short The geomagnetic solar flare effect identified by SIIG as an indicator of a solar flare observed by GOES satellites
title_full The geomagnetic solar flare effect identified by SIIG as an indicator of a solar flare observed by GOES satellites
title_fullStr The geomagnetic solar flare effect identified by SIIG as an indicator of a solar flare observed by GOES satellites
title_full_unstemmed The geomagnetic solar flare effect identified by SIIG as an indicator of a solar flare observed by GOES satellites
title_sort The geomagnetic solar flare effect identified by SIIG as an indicator of a solar flare observed by GOES satellites
dc.creator.none.fl_str_mv Van Zele, Maria Andrea
Meza, A.
author Van Zele, Maria Andrea
author_facet Van Zele, Maria Andrea
Meza, A.
author_role author
author2 Meza, A.
author2_role author
dc.subject.none.fl_str_mv Solar flare effect
Geomagnetic field
GPS
Total electron content
topic Solar flare effect
Geomagnetic field
GPS
Total electron content
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.5
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv This paper studies the efficiency of geomagnetic solar flare effects (gsfe) in X solar flare detection; so during the period 1999?2007 a comparison between solar flare (sf) observed by satellites of the Geostationary Operational Environmental Satellite (GOES) programme and gsfe published by the Service International des Indices Geomagnetiques (SIIG) is made.Solar flares (sfs) are one of the most powerful manifestations of the solar activity. Because the far UV and soft and hard X-ray solar flare radiation is absorbed by the ionosphere, the ionized gas density increases (ionospheric solar flare effect, isfe) and a sudden enhancement of geomagnetic field near Earth surface (geomagnetic solar flare effect, gsfe) is produced.The solar X-ray flux is systematically recorded since 1975 by GOES satellites, and gsfe are declared by geomagnetic observatories since 1957. We corroborate that the identification of sf using gsfe is affected by several factors:? the intensity and average growth rate of solar flare radiation when quicker is it more easily the sf is detected as gsfe;? the position of the geomagnetic observatory, we found that observatories placed at summer hemisphere identify more easily the sf, sothe uneven geographical distribution of observatories make the sf identification difficult;? the existing geomagnetic perturbation previous to sf, and the likeness between the gsfe and other geomagnetic variations.This work shows that gsfe recorded as associated to sf is a poor detector of sf even if it is intense. Some of these inconveniences can be avoided if the distribution of the observatories is improved and the identification of a sf is made using simultaneously gsfe, solar wind parameters and isfe.
Fil: Van Zele, Maria Andrea. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Departamento de Geología; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Geociencias Básicas, Aplicadas y Ambientales de Buenos Aires. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Geociencias Básicas, Aplicadas y Ambientales de Buenos Aires; Argentina
Fil: Meza, A.. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina
description This paper studies the efficiency of geomagnetic solar flare effects (gsfe) in X solar flare detection; so during the period 1999?2007 a comparison between solar flare (sf) observed by satellites of the Geostationary Operational Environmental Satellite (GOES) programme and gsfe published by the Service International des Indices Geomagnetiques (SIIG) is made.Solar flares (sfs) are one of the most powerful manifestations of the solar activity. Because the far UV and soft and hard X-ray solar flare radiation is absorbed by the ionosphere, the ionized gas density increases (ionospheric solar flare effect, isfe) and a sudden enhancement of geomagnetic field near Earth surface (geomagnetic solar flare effect, gsfe) is produced.The solar X-ray flux is systematically recorded since 1975 by GOES satellites, and gsfe are declared by geomagnetic observatories since 1957. We corroborate that the identification of sf using gsfe is affected by several factors:? the intensity and average growth rate of solar flare radiation when quicker is it more easily the sf is detected as gsfe;? the position of the geomagnetic observatory, we found that observatories placed at summer hemisphere identify more easily the sf, sothe uneven geographical distribution of observatories make the sf identification difficult;? the existing geomagnetic perturbation previous to sf, and the likeness between the gsfe and other geomagnetic variations.This work shows that gsfe recorded as associated to sf is a poor detector of sf even if it is intense. Some of these inconveniences can be avoided if the distribution of the observatories is improved and the identification of a sf is made using simultaneously gsfe, solar wind parameters and isfe.
publishDate 2011
dc.date.none.fl_str_mv 2011-09
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/11336/280060
Van Zele, Maria Andrea; Meza, A.; The geomagnetic solar flare effect identified by SIIG as an indicator of a solar flare observed by GOES satellites; Elsevier; Advances in Space Research; 48; 5; 9-2011; 826-836
0273-1177
CONICET Digital
CONICET
url http://hdl.handle.net/11336/280060
identifier_str_mv Van Zele, Maria Andrea; Meza, A.; The geomagnetic solar flare effect identified by SIIG as an indicator of a solar flare observed by GOES satellites; Elsevier; Advances in Space Research; 48; 5; 9-2011; 826-836
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/url/https://www.sciencedirect.com/science/article/abs/pii/S0273117711003103
info:eu-repo/semantics/altIdentifier/doi/10.1016/j.asr.2011.04.037
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 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 13.106097

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