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Tipo da ReferênciaConference Proceedings
Repositóriosid.inpe.br/mtc-m17@80/2007/12.17.14.27
Metadadossid.inpe.br/mtc-m17@80/2007/12.17.14.27.03
Sitemtc-m16b.sid.inpe.br
Chave SecundáriaINPE--PRE/
Código do Detentorisadg {BR SPINPE} ibi 8JMKD3MGPCW/3DT298S
Chave de CitaçãoWrasseEcheDalLFech:2007:HiSpSt
Autor1 Wrasse, Cristiano Max
2 Echer, Ezequiel
3 Dal Lago, Alisson
4 Fechine, Joaquim
Grupo1
2 DGE-INPE-MCT-BR
3 DGE-INPE-MCT-BR
4 DGE-INPE-MCT-BR
Afiliação1 UNIVAP
2 Instituto Nacional de Pesquisas Espaciais (INPE)
3 Instituto Nacional de Pesquisas Espaciais (INPE)
4 Instituto Nacional de Pesquisas Espaciais (INPE)
TítuloHigh speed streams and geomagnetic activity recurrency during different solar cycles revealed by wavelet analysis
Nome do EventoEncontro Brasileiro de Física dos Plasmas, 9.
Ano2007
Data25-28 Nov.
Localização do EventoSão Pedro, SP
ResumoSolar wind velocity and the geomagnetic index Ap are used to verify the recurrency of the high speed streams and the geomagnetic activity in di®erent solar cycles. The wavelet technique is used to perform the spectral analysis of the solar wind velocity, interplanetary magnetic ¯eld parameters and geomagnetic index with 1-day resolution. The Ap index between 1978 and 2003 is also used. The solar wind velocity data come from three di®erent instruments in order to access di®erent time periods and solar cycles. The ISEE-3 is used for the period of 1978-1982. The WIND satellite is used for 1995-1997 and the ACE satellite is used for 1998-2002 period. The results suggest that the semi-annual variation in Ap index is stronger during descending phase of the solar cycle, while the annual variation in Ap is stronger during solar cycle 22 (1989-1990) maximum than during solar cycles 21 and 23. It is also observed that the 27-day periodicity is stronger for ~B components than for ~V components around 1998-2002. A semi-annual variation is clearly observed in ~V components than in ~B components around 1998-2002. Regarding the 27-day variation in solar wind speed and magnetic ¯eld strength, it can be seen that this periodicity is more visible in ~V than in ~B . This periodicity is also more stable (it exists for more time) during the 1995-1997 minimum than during the 1978-1982 maximum.
Idiomapt
Tipo SecundárioPRE CN
Tipo TerciárioPoster
AreaCEA
Última Atualização dos Metadados2018:06.05.03.36.36 cptec.inpe.br/walmeida/2003/04.25.17.12 administrator {D 2007}
Estágio do Documentoconcluido
e-Mail (login)marciana
Grupo de Usuáriosadministrator
simone
administrator
Visibilidadeshown
Transferível1
Acervo Hospedeirolcp.inpe.br/ignes/2004/02.12.18.39
cptec.inpe.br/walmeida/2003/04.25.17.12
Tipo do ConteudoExternal Contribution
Unidades Imediatamente Superiores8JMKD3MGPCW/3EU29DP
Conteúdo da Pasta sourcenão têm arquivos
Conteúdo da Pasta agreementnão têm arquivos
Histórico2007-12-17 14:27:03 :: simone -> administrator ::
2012-10-24 00:13:46 :: administrator -> simone ::
2013-02-20 15:20:15 :: simone -> administrator :: 2007
2018-06-05 03:36:36 :: administrator -> marciana :: 2007
Campos Vaziosaccessionnumber archivingpolicy archivist booktitle callnumber copyholder copyright creatorhistory descriptionlevel dissemination documentstage doi e-mailaddress edition editor electronicmailaddress format isbn issn keywords label lineage mark mirrorrepository nextedition notes numberoffiles numberofvolumes orcid organization pages parameterlist parentrepositories previousedition previouslowerunit progress project publisher publisheraddress readergroup readpermission resumeid rightsholder secondarydate secondarymark serieseditor session shorttitle size sponsor subject targetfile tertiarymark type url versiontype volume
Data de Acesso17 fev. 2020
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