Solar and interplanetary origins of the November 2004 superstorms

Autor(es)

Echer, Ezequiel ^[1] ; Tsurutani, Bruce T. ^[2] ; Guarnieri, Fernando L. ^[3]

Afiliação do(s) autor(es)

^[1] INPE, Sao Jose Dos Campos, SP - Brazil

^[2] CALTECH, Jet Prop Lab, Pasadena, CA - USA

^[3] Univ Vale Paraiba UNIVAP, Sao Jose Dos Campos, SP - Brazil

• Tipo de documento: Artigo Científico
• Fonte: Advances in Space Research; v. 44, n. 5, p. 615-620, SEP 1 2009.
• Citações Web of Science: 4

Resumo

During the first half of November 2004, many solar flares and coronal mass ejections (CMEs) were associated with solar active region (AR) 10696. This paper attempts to identify the solar and interplanetary origins of two superstorms which occurred on 8 and 10 November with peak intensities of Dst = -373 nT and -289 nT, respectively. Southward interplanetary magnetic fields within a magnetic cloud (MC), and a sheath + MC were the causes of these two superstorms, respectively. Two different CME propagation models {[}Gopalswamy, N., Yashiro, S., Kaiser, M.L. et al. Predicting the 1-AU arrival times of coronal mass ejections. J. Geophys. Res. 106, 29207-29219, 2001; Gopalswamy, N.S., Lara, A., Manoharan, P.K. et al. An empirical model to predict the 1-AU arrival of interplanetary shocks. Adv. Space Res. 36, 2289-2294, 2005] were employed to attempt to identify the solar sources. It is found that the models identify several potential CMEs as possible sources for each of the superstorms. The two Gopalswamy et al. models give the possible sources for the first superstorm as CMEs on 2330 UT 4 November 2004 or on 1454 UT 5 November 2004. For the second superstorm, the possible solar source was a CME that on 0754 UT 5 November 2004 or one that occurred on 1206 UT 5 November 2004. We note that other propagation models sometimes agree and other times disagree with the above results. It is concluded that during high solar/interplanetary activity intervals such as this one, the exact solar source is difficult to identify. More refined propagation models are needed. (C) 2009 COSPAR. Published by Elsevier Ltd. All rights reserved. (AU)

• Processo FAPESP: 08/05607-2 - Bruce Tadashi Tsurutani | Jet Propulsion Laboratory/NASA - Estados Unidos
• Beneficiário: Fernando Luis Guarnieri
• Modalidade de apoio: Auxílio à Pesquisa - Pesquisador Visitante - Internacional