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Tipo de ReferênciaJournal Article
Sitemtc-m16d.sid.inpe.br
Código do Detentorisadg {BR SPINPE} ibi 8JMKD3MGPCW/3DT298S
Identificador8JMKD3MGP7W/37JT9U2
Repositóriosid.inpe.br/mtc-m19@80/2010/06.01.14.06   (acesso restrito)
Última Atualização2010:06.01.14.06.27 (UTC) administrator
Metadadossid.inpe.br/mtc-m19@80/2010/06.01.14.06.29
Última Atualização dos Metadados2021:07.18.04.02.29 (UTC) administrator
Chave SecundáriaINPE--PRE/
DOI10.1016/j.jastp.2010.04.003
ISSN1364-6826
Chave de CitaçãoTsurutaniEcheGuarGonz:2011:PrTwSo
TítuloThe properties of two solar wind high speed streams and related geomagnetic activity during the declining phase of solar cycle 23
Ano2011
MêsJan.
Data de Acesso25 jul. 2021
Número de Arquivos1
Tamanho2175 KiB
Área de contextualização
Autor1 Tsurutani, Bruce T.
2 Echer, Ezequiel
3 Guarnieri, Fernando L.
4 Gonzalez Alarcon, Walter Demétrio
Identificador de Curriculo1
2 8JMKD3MGP5W/3C9JH3D
3
4 8JMKD3MGP5W/3C9JJC4
Grupo1
2 DGE-CEA-INPE-MCT-BR
3
4 DAS-CEA-INPE-MCT-BR
Afiliação1 CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA
2 Instituto Nacional de Pesquisas Espaciais (INPE)
3 Universidade do Vale do Paraiba (UNIVAP)
4 Instituto Nacional de Pesquisas Espaciais (INPE)
RevistaJournal of Atmospheric and Solar-Terrestrial Physics
Volume73
Número1
Páginas164-177
Tipo SecundárioPRE PI
Nota SecundáriaB2_ASTRONOMIA_/_FÍSICA B1_CIÊNCIAS_BIOLÓGICAS_I B1_ECOLOGIA_E_MEIO_AMBIENTE B1_ENGENHARIAS_IV B1_GEOCIÊNCIAS A2_INTERDISCIPLINAR
Histórico (UTC)2010-07-05 14:54:45 :: simone -> marciana :: 2010
2011-02-23 13:14:59 :: marciana :: 2010 -> 2011
2011-08-04 14:46:51 :: marciana -> administrator :: 2011
2011-11-07 05:50:29 :: administrator -> marciana :: 2011
2011-11-10 13:00:38 :: marciana -> administrator :: 2011
2021-07-18 04:02:29 :: administrator -> tereza@sid.inpe.br :: 2011
Área de conteúdo e estrutura
É a matriz ou uma cópia?é a matriz
Estágio do Conteúdoconcluido
Transferível1
Tipo do ConteudoExternal Contribution
Tipo de Versãopublisher
Palavras-ChaveHigh speed solar wind streams, Interplanetary Alfvenicity, Geomagnetic activity, HILDCAAs.
ResumoTwo high speed stream (HSS) solar wind intervals (days 283¨C294 and 314¨C318, 2003, hereafter called Events 1 and 2) during the declining phase of solar cycle 23 have been examined in detail for their interplanetary characteristics and their resultant geomagnetic activity. Event 1 had an associated storm initial phase with peak Dst=+9 nT. This was caused by a high plasma density heliospheric plasma sheet (HPS) which impacted the magnetosphere. The southward component of IMF Bz fluctuations in the corotating interaction regions (CIRs) of both Events 1 and 2 led to peak storm main phases of Dst=−85 and −62 nT, respectively. The extended storm ¡°recovery¡± phases were associated with ¦¤B/Bo 1¨C2 Alfv¨¦nic fluctuations in the HSS proper. High-intensity, long-duration, continuous AE (HILDCAA) intervals were present, presumably due to the southward component of the Alfv¨¦n waves. The IMF Bx¨CVx 4-h cross-correlation values were >0.8 in Event 2, and lower, >0.6, in Event 1. The difference in Alfv¨¦nicity between the two HSS events is not understood at present. The IMF Bz 10-min to 3-h variances and are highest during the CIRs. The normalized variances during the HSS proper are approximately the same as those for the CIRs. For Event 1, the 1-h IMF and are 5.0 nT2 and 1.1¡Á10−1, respectively. The IMF Bz-AE cross-correlation (c.c.) coefficients during the storm main phase of Event 1 and for 24-h of the HSS of Event 2 give similar results. For the Event 1, a peak c.c. of −0.4 occurred with a lag of 103 min, and for Event 2 a peak c.c of −0.38 with a lag of 67 min was obtained. Both c.c. results were sharply peaked. The decay-portion of a HSS prior to Event 1 was characterized by low Np, low Bo and low Alfv¨¦n wave amplitudes. The 1-h IMF and were 0.84 nT2 and 2.9¡Á10−2, respectively. This quiet interplanetary interval led to a quiet geomagnetic activity period (AE<100 nT, Dst +5 nT). On the other hand, what is quite surprising is that this region was the most purely ¡°Alfv¨¦nic¡± interval studied (c.c. of Bx-Vx=0.95).The ¦Å parameter was calculated using both GSE and GSM coordinates. It was found that ¦Å is 30% larger for GSM coordinates. Thus, the major cause of geomagnetic activity during HSSs is the large amplitude Alfv¨¦n waves but not coordinate transformations. Sector polarities (IMF By values) may be a secondary factor. However, other models, like the tilted solar dipole, should be considered as well.
AreaCEA
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Unidades Imediatamente Superiores8JMKD3MGPCW/3ETR8EH
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DivulgaçãoWEBSCI; PORTALCAPES; AGU; MGA; COMPENDEX.
Acervo Hospedeirosid.inpe.br/mtc-m19@80/2009/08.21.17.02
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