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1. Identificação
Tipo de ReferênciaArtigo em Revista Científica (Journal Article)
Sitemarte3.sid.inpe.br
Código do Detentorisadg {BR SPINPE} ibi 8JMKD3MGPCW/3DT298S
Identificador6qtX3pFwXQZ3r59YCT/GUipr
Repositóriosid.inpe.br/iris@1905/2005/07.29.02.07   (acesso restrito)
Última Atualização2015:08.18.15.22.11 (UTC) marciana
Repositório de Metadadossid.inpe.br/iris@1905/2005/07.29.02.07.34
Última Atualização dos Metadados2018:06.06.04.14.27 (UTC) administrator
Chave SecundáriaINPE-5096-PRE/1598
ISSN0038-0938
1573-093X
Rótulo2958
Chave de CitaçãoSawantLattBenzDenn:1990:HaXrAs
TítuloHard X-rays associated weak decimetric bursts
Ano1990
Data Secundária1990322
Data de Acesso20 maio 2024
Tipo SecundárioPRE PI
Número de Arquivos1
Tamanho810 KiB
2. Contextualização
Autor1 Sawant, Hanumant Shankar
2 Lattari, C. J. B.
3 Benz, A. O.
4 Dennis, B. R
Grupo1 DAS-INPE-BR
RevistaSolar Physics
Volume130
Número1-2
Páginas57-73
Histórico (UTC)2014-09-29 15:13:34 :: administrator -> marciana :: 1990
2015-08-18 15:22:11 :: marciana -> administrator :: 1990
2018-06-06 04:14:27 :: administrator -> marciana :: 1990
3. Conteúdo e estrutura
É a matriz ou uma cópia?é a matriz
Estágio do Conteúdoconcluido
Transferível1
Tipo do ConteúdoExternal Contribution
Palavras-ChaveASTROFISICA
ResumoIn previous attempts to show one-to-one correlation between type III bursts and X-ray spikes, there have been ambiguities as to which of several X-rays spikes are correlated with any given type III burst. Here, we present observations that show clear associations of X-ray bursts with RS type III bursts between 16:46 UT and 16:52 UT on July 9, 1985. The hard X-ray observations were made at energies above 25 keV with HXRBS on SMM and the radio observations were made at 1.63 GHz using the 13.7 m Itapetinga antenna in R and L polarization with a time resolution of 3 ms. Detailed comparison between the hard X-ray and radio observations shows: (1) In at least 13 cases we can identify the associated hard X-ray and decimetric RS bursts. (2) On average, the X-ray peaks were delayed from the peak of the RS bursts at 1.6 GHz by 400 ms although a delay as long as 1 s was observed in one case. One possible explanation of the long delays between the RS bursts and the associated X-ray is that RS bursts is produced at the leading edge of the electron beam, whereas the X-ray burst peaks at the time of arrival of the bulk of the electrons at the high density region at the lower corona and upper chromosphere. Thus, the time comparison must be made between the peak of the radio pulse and the start of the X-ray burst. In that case the delays are consistent with an electron travel time with velocity 0.3 c from the 800 MHz plasma level to the lower corona assuming that the radio emission is at the second harmonic.
ÁreaCEA
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Conteúdo da Pasta agreementnão têm arquivos
4. Condições de acesso e uso
Arquivo Alvo5096.pdf
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Grupo de Leitoresadministrator
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Visibilidadeshown
Política de Arquivamentodenypublisher denyfinaldraft12
Permissão de Leituradeny from all and allow from 150.163
Permissão de Atualizaçãonão transferida
5. Fontes relacionadas
Unidades Imediatamente Superiores8JMKD3MGPCW/3ETR8EH
DivulgaçãoWEBSCI; PORTALCAPES.
Acervo Hospedeirosid.inpe.br/banon/2001/04.03.15.36
6. Notas
Campos Vaziosaffiliation alternatejournal archivist callnumber copyholder copyright creatorhistory descriptionlevel doi e-mailaddress electronicmailaddress format isbn language lineage mark mirrorrepository month nextedition notes orcid parameterlist parentrepositories previousedition previouslowerunit progress project resumeid rightsholder schedulinginformation secondarymark session shorttitle sponsor subject tertiarymark tertiarytype typeofwork url versiontype
7. Controle da descrição
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