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1. Identificação
Tipo de ReferênciaArtigo em Revista Científica (Journal Article)
Sitemtc-m16b.sid.inpe.br
Código do Detentorisadg {BR SPINPE} ibi 8JMKD3MGPCW/3DT298S
Identificador6qtX3pFwXQZGivnK2Y/UuLwP
Repositóriosid.inpe.br/mtc-m17@80/2008/06.18.12.23   (acesso restrito)
Última Atualização2008:06.18.12.23.11 (UTC) administrator
Repositório de Metadadossid.inpe.br/mtc-m17@80/2008/06.18.12.23.13
Última Atualização dos Metadados2018:06.05.03.30.52 (UTC) administrator
Chave SecundáriaINPE--PRE/
DOI10.1007/s11207-008-9185-9
ISSN0038-0938
1573-093X
Chave de CitaçãoKane:2008:GnPeGa
TítuloGnevyshev Peaks and Gaps for Coronal Mass Ejections of Different Widths Originating in Different Solar Position Angles
Ano2008
MêsJune
Data de Acesso07 maio 2024
Tipo SecundárioPRE PI
Número de Arquivos1
Tamanho511 KiB
2. Contextualização
AutorKane, Rajaram Purushotam
GrupoDGE-CEA-INPE-MCT-BR
AfiliaçãoInstituto Nacional de Pesquisas Espaciais (INPE)
RevistaSolar Physics
Volume249
Número2
Páginas369-380
Histórico (UTC)2008-06-18 12:23:13 :: simone -> administrator ::
2012-07-13 22:33:07 :: administrator -> simone ::
2013-02-20 15:20:20 :: simone -> administrator :: 2008
2018-06-05 03:30:52 :: administrator -> marciana :: 2008
3. Conteúdo e estrutura
É a matriz ou uma cópia?é a matriz
Estágio do Conteúdoconcluido
Transferível1
Tipo do ConteúdoExternal Contribution
ResumoThe sunspot number series at the peak of sunspot activity often has two or three peaks (Gnevyshev peaks; Gnevyshev, Solar Phys. 1, 107, 1967; Solar Phys. 51, 175, 1977). The sunspot group number (SGN) data were examined for 1997  2003 (part of cycle 23) and compared with data for coronal mass ejection (CME) events. It was noticed that they exhibited mostly two Gnevyshev peaks in each of the four latitude belts 0°  10°, 10°  20°, 20 °  30°, and > 30°, in both N (northern) and S (southern) solar hemispheres. The SGN were confined to within latitudes ± 50° around the Equator, mostly around ± 35°, and seemed to occur later in lower latitudes, indicating possible latitudinal migration as in the Maunder butterfly diagrams. In CMEs, less energetic CMEs (of widths < 71°) showed prominent Gnevyshev peaks during sunspot maximum years in almost all latitude belts, including near the poles. The CME activity lasted longer than the SGN activity. However, the CME peaks did not match the SGN peaks and were almost simultaneous at different latitudes, indicating no latitudinal migration. In energetic CMEs including halo CMEs, the Gnevyshev peaks were obscure and ill-defined. The solar polar magnetic fields show polarity reversal during sunspot maximum years, first at the North Pole and, a few months later, at the South Pole. However, the CME peaks and gaps did not match with the magnetic field reversal times, preceding them by several months, rendering any cause  effect relationship doubtful.
ÁreaCEA
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Conteúdo da Pasta docacessar
Conteúdo da Pasta sourcenão têm arquivos
Conteúdo da Pasta agreementnão têm arquivos
4. Condições de acesso e uso
Idiomaen
Arquivo Alvognevyshev.pdf
Grupo de Usuáriosadministrator
simone
Visibilidadeshown
Política de Arquivamentodenypublisher denyfinaldraft12
Permissão de Leituradeny from all and allow from 150.163
5. Fontes relacionadas
Unidades Imediatamente Superiores8JMKD3MGPCW/3EU29DP
DivulgaçãoWEBSCI; PORTALCAPES.
Acervo Hospedeirolcp.inpe.br/ignes/2004/02.12.18.39
cptec.inpe.br/walmeida/2003/04.25.17.12
6. Notas
Campos Vaziosalternatejournal archivist callnumber copyholder copyright creatorhistory descriptionlevel documentstage e-mailaddress electronicmailaddress format isbn keywords label lineage mark mirrorrepository nextedition notes orcid parameterlist parentrepositories previousedition previouslowerunit progress project readergroup resumeid rightsholder schedulinginformation secondarydate secondarymark session shorttitle sponsor subject tertiarymark tertiarytype typeofwork url versiontype
7. Controle da descrição
e-Mail (login)marciana
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