Characteristics of coronal mass ejections in the near Sun interplanetary space

Based on the observations from the Large Angle and Spectrometric Coronagraph (LASCO) on board the Solar and Heliospheric Observatory (SOHO) spacecraft we studied coronal mass ejections (CME) parameters between 6 and 10 solar radii from the Sun. We have developed a new method to obtain the duration,...

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Detalles Bibliográficos
Autores: Lara Sanchez, Alejandro, González-Esparza, J. Américo, Gopalswamy, Nat
Tipo de recurso: artículo
Estado:Versión publicada
Fecha de publicación:2004
País:México
Institución:UNIVERSIDAD NACIONAL AUTÓNOMA DE MÉXICO
Repositorio:Geofísica Internacional
Idioma:español
inglés
OAI Identifier:oai:revistagi.geofisica.unam.mx:article/921
Acceso en línea:http://revistagi.geofisica.unam.mx/index.php/RGI/article/view/921
Access Level:acceso abierto
Palabra clave:Eyecciones de Masa Coronal
actividad solar
Coronal Mass Ejections
solar activity
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spelling Characteristics of coronal mass ejections in the near Sun interplanetary spaceCharacteristics of coronal mass ejections in the near Sun interplanetary spaceLara Sanchez, AlejandroGonzález-Esparza, J. AméricoGopalswamy, NatEyecciones de Masa Coronalactividad solarCoronal Mass Ejectionssolar activityBased on the observations from the Large Angle and Spectrometric Coronagraph (LASCO) on board the Solar and Heliospheric Observatory (SOHO) spacecraft we studied coronal mass ejections (CME) parameters between 6 and 10 solar radii from the Sun. We have developed a new method to obtain the duration, brightness enhancement (above the background) and speed of the leading part of the CMEs. These properties are important in order to understand the dynamics of the CMEs near the Sun and their evolution in the interplanetary space using numerical models. We present the method of analysis and the results of the application of this method to a set of 9 halo CMEs observed during 1997. We found that i) the CME speeds obtained with this method are in good agreement with measurements of other observers, ii) the average time duration of the CME leading part is 8 hrs. and iii) the brightness maxima decrease with distance as a power law with a mean index of -3.6.Con base en las observaciones del Coronógrafo Espectrométrico de Gran Angular (LASCO) que se encuentra a bordo del Observatorio Solar y Heliosférico (SOHO) estudiamos algunos parámetros de las Eyecciones de Masa Coronal (CME) a distancias de 6 a 10 radios solares. Desarrollamos un método nuevo para calcular la duración, el incremento del brillo (sobre el nivel de fondo) y la velocidad de la estructura delantera de las eyecciones. Estas propiedades son importantes para entender la dinámica de las eyecciones cerca del Sol y son también críticas para estudiar su evolución en el medio interplanetario usando modelos numéricos. En este trabajo presentamos el método de análisis y los resultados de la aplicación de este método a un grupo de 9 eyecciones tipo halo observadas durante 1997. Encontramos que i) la velocidad de las eyecciones obtenida con este método coincide con las mediciones de otros observadores ii) la duración promedio de la parte delantera de las eyecciones es de 8 hrs, y iii) la brillantez máxima decrece con la distancia como una ley de potencias con índice promedio de -3.6.Universidad Nacional Autónoma de México. Instituto de Geofísica2004-01-01info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionapplication/pdfhttp://revistagi.geofisica.unam.mx/index.php/RGI/article/view/92110.22201/igeof.00167169p.2004.43.1.216Geofisica Internacional; Vol. 43 No. 1 (2004): January 1, 2004; 75-82Geofísica Internacional; Vol. 43 Núm. 1 (2004): Enero 1, 2004; 75-822954-436X0016-716910.22201/igeof.00167169p.2004.43.1reponame:Geofísica Internacionalinstname:UNIVERSIDAD NACIONAL AUTÓNOMA DE MÉXICOinstacron:UNAMspaenghttp://revistagi.geofisica.unam.mx/index.php/RGI/article/view/921/872http://revistagi.geofisica.unam.mx/index.php/RGI/article/view/921/2605https://creativecommons.org/licenses/by-nc-sa/4.0/info:eu-repo/semantics/openAccessoai:revistagi.geofisica.unam.mx:article/9212024-08-16T17:32:01Z
dc.title.none.fl_str_mv Characteristics of coronal mass ejections in the near Sun interplanetary space
Characteristics of coronal mass ejections in the near Sun interplanetary space
title Characteristics of coronal mass ejections in the near Sun interplanetary space
spellingShingle Characteristics of coronal mass ejections in the near Sun interplanetary space
Lara Sanchez, Alejandro
Eyecciones de Masa Coronal
actividad solar
Coronal Mass Ejections
solar activity
title_short Characteristics of coronal mass ejections in the near Sun interplanetary space
title_full Characteristics of coronal mass ejections in the near Sun interplanetary space
title_fullStr Characteristics of coronal mass ejections in the near Sun interplanetary space
title_full_unstemmed Characteristics of coronal mass ejections in the near Sun interplanetary space
title_sort Characteristics of coronal mass ejections in the near Sun interplanetary space
dc.creator.none.fl_str_mv Lara Sanchez, Alejandro
González-Esparza, J. Américo
Gopalswamy, Nat
author Lara Sanchez, Alejandro
author_facet Lara Sanchez, Alejandro
González-Esparza, J. Américo
Gopalswamy, Nat
author_role author
author2 González-Esparza, J. Américo
Gopalswamy, Nat
author2_role author
author
dc.subject.none.fl_str_mv Eyecciones de Masa Coronal
actividad solar
Coronal Mass Ejections
solar activity
topic Eyecciones de Masa Coronal
actividad solar
Coronal Mass Ejections
solar activity
description Based on the observations from the Large Angle and Spectrometric Coronagraph (LASCO) on board the Solar and Heliospheric Observatory (SOHO) spacecraft we studied coronal mass ejections (CME) parameters between 6 and 10 solar radii from the Sun. We have developed a new method to obtain the duration, brightness enhancement (above the background) and speed of the leading part of the CMEs. These properties are important in order to understand the dynamics of the CMEs near the Sun and their evolution in the interplanetary space using numerical models. We present the method of analysis and the results of the application of this method to a set of 9 halo CMEs observed during 1997. We found that i) the CME speeds obtained with this method are in good agreement with measurements of other observers, ii) the average time duration of the CME leading part is 8 hrs. and iii) the brightness maxima decrease with distance as a power law with a mean index of -3.6.
publishDate 2004
dc.date.none.fl_str_mv 2004-01-01
dc.type.none.fl_str_mv info:eu-repo/semantics/article
info:eu-repo/semantics/publishedVersion
format article
status_str publishedVersion
dc.identifier.none.fl_str_mv http://revistagi.geofisica.unam.mx/index.php/RGI/article/view/921
10.22201/igeof.00167169p.2004.43.1.216
url http://revistagi.geofisica.unam.mx/index.php/RGI/article/view/921
identifier_str_mv 10.22201/igeof.00167169p.2004.43.1.216
dc.language.none.fl_str_mv spa
eng
language spa
eng
dc.relation.none.fl_str_mv http://revistagi.geofisica.unam.mx/index.php/RGI/article/view/921/872
http://revistagi.geofisica.unam.mx/index.php/RGI/article/view/921/2605
dc.rights.none.fl_str_mv https://creativecommons.org/licenses/by-nc-sa/4.0/
info:eu-repo/semantics/openAccess
rights_invalid_str_mv https://creativecommons.org/licenses/by-nc-sa/4.0/
eu_rights_str_mv openAccess
dc.format.none.fl_str_mv application/pdf
dc.publisher.none.fl_str_mv Universidad Nacional Autónoma de México. Instituto de Geofísica
publisher.none.fl_str_mv Universidad Nacional Autónoma de México. Instituto de Geofísica
dc.source.none.fl_str_mv Geofisica Internacional; Vol. 43 No. 1 (2004): January 1, 2004; 75-82
Geofísica Internacional; Vol. 43 Núm. 1 (2004): Enero 1, 2004; 75-82
2954-436X
0016-7169
10.22201/igeof.00167169p.2004.43.1
reponame:Geofísica Internacional
instname:UNIVERSIDAD NACIONAL AUTÓNOMA DE MÉXICO
instacron:UNAM
instname_str UNIVERSIDAD NACIONAL AUTÓNOMA DE MÉXICO
instacron_str UNAM
institution UNAM
reponame_str Geofísica Internacional
collection Geofísica Internacional
repository.name.fl_str_mv
repository.mail.fl_str_mv
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