| 1. Identificação | |
| Tipo de Referência | Artigo em Revista Científica (Journal Article) |
| Site | mtc-m21b.sid.inpe.br |
| Código do Detentor | isadg {BR SPINPE} ibi 8JMKD3MGPCW/3DT298S |
| Identificador | 8JMKD3MGP5W34M/3HE6STN |
| Repositório | sid.inpe.br/mtc-m21b/2014/11.19.02.18.29 |
| Última Atualização | 2015:01.16.13.26.00 (UTC) administrator |
| Repositório de Metadados | sid.inpe.br/mtc-m21b/2014/11.19.02.18.30 |
| Última Atualização dos Metadados | 2018:06.04.03.04.35 (UTC) administrator |
| DOI | 10.1088/0004-637X/793/1/6 |
| ISSN | 0004-637X 1538-4357 |
| Rótulo | isi 2014-11 RemyaTsReLaFaEcGl:2014:LOPLBe |
| Chave de Citação | RemyaTsReLaFaEcGl:2014:LoPlBe |
| Título | Large-amplitude, circularly polarized, compressive, obliquely propagating electromagnetic proton cyclotron waves throughout the earth's magnetosheath: low plasma beta conditions  |
| Ano | 2014 |
| Mês | Sep. |
| Data de Acesso | 25 abr. 2024 |
| Tipo Secundário | PRE PI |
| Número de Arquivos | 1 |
| Tamanho | 1609 KiB |
| 2. Contextualização | |
| Autor | 1 Remya, B. 2 Tsurutani, B. T. 3 Reddy, R. V. 4 Lakhina, G. S. 5 Falkowski, B. J. 6 Echer, Ezequiel 7 Glassmeier, K. -H. |
| Identificador de Curriculo | 1 2 3 4 5 6 8JMKD3MGP5W/3C9JH3D |
| Grupo | 1 2 3 4 5 6 DGE-CEA-INPE-MCTI-GOV-BR |
| Afiliação | 1 Indian Inst Geomagnetism, Navi Mumbai, Maharashtra, India. 2 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. 3 Indian Inst Geomagnetism, Navi Mumbai, Maharashtra, India. 4 Indian Inst Geomagnetism, Navi Mumbai, Maharashtra, India. 5 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. 6 Instituto Nacional de Pesquisas Espaciais (INPE) 7 IGEP, D-38106 Braunschweig, Germany. |
| Endereço de e-Mail | marcelo.pazos@inpe.br |
| Revista | Astrophysical Journal |
| Volume | 793 |
| Número | 1 |
| Histórico (UTC) | 2018-06-04 03:04:35 :: administrator -> marciana :: 2014 |
| 3. Conteúdo e estrutura | |
| É a matriz ou uma cópia? | é a matriz |
| Estágio do Conteúdo | concluido |
| Transferível | 1 |
| Tipo do Conteúdo | External Contribution |
| Tipo de Versão | publisher |
| Palavras-Chave | instabilities methods: data analysis planets and satellites: individual (Earth Cassini WIND) planets and satellites: magnetic fields polarization |
| Resumo | During 1999 August 18, both Cassini and WIND were in the Earth's magnetosheath and detected transverse electromagnetic waves instead of the more typical mirror-mode emissions. The Cassini wave amplitudes were as large as similar to 14 nT (peak to peak) in a similar to 55 nT ambient magnetic field B-0. A new method of analysis is applied to study these waves. The general wave characteristics found were as follows. They were left-hand polarized and had frequencies in the spacecraft frame (f(scf)) below the proton cyclotron frequency (f(p)). Waves that were either right-hand polarized or had f(scf) > f(p) are shown to be consistent with Doppler-shifted left-hand waves with frequencies in the plasma frame f(pf) < f(p). Thus, almost all waves studied are consistent with their being electromagnetic proton cyclotron waves. Most of the waves (similar to 55\%) were found to be propagating along B0 (theta(kB0) < 30 degrees), as expected from theory. However, a significant fraction of the waves were found to be propagating oblique to B0. These waves were also circularly polarized. This feature and the compressive ([B-max - B-min]/B-max, where B-max and B-min are the maximum and minimum field magnitudes) nature (ranging from 0.27 to 1.0) of the waves are noted but not well understood at this time. The proton cyclotron waves were shown to be quasi-coherent, theoretically allowing for rapid pitch-angle transport of resonant protons. Because Cassini traversed the entire subsolar magnetosheath and WIND was in the dusk-side flank of the magnetosheath, it is surmised that the entire region was filled with these waves. In agreement with past theory, it was the exceptionally low plasma beta (0.35) that led to the dominance of the proton cyclotron wave generation during this interval. A high-speed solar wind stream (< V-sw > = 598 km s(-1)) was the source of this low-beta plasma. |
| Área | CEA |
| Arranjo | urlib.net > BDMCI > Fonds > Produção anterior à 2021 > DIDGE > Large-amplitude, circularly polarized,... |
| Conteúdo da Pasta doc | acessar |
| Conteúdo da Pasta source | não têm arquivos |
| Conteúdo da Pasta agreement | não têm arquivos |
| 4. Condições de acesso e uso | |
| URL dos dados | http://urlib.net/ibi/8JMKD3MGP5W34M/3HE6STN |
| URL dos dados zipados | http://urlib.net/zip/8JMKD3MGP5W34M/3HE6STN |
| Idioma | en |
| Arquivo Alvo | 0004-637X_793_1_6remya.pdf |
| Grupo de Usuários | administrator marcelo.pazos@inpe.br marciana |
| Grupo de Leitores | administrator marcelo.pazos@inpe.br marciana |
| Visibilidade | shown |
| Política de Arquivamento | allowpublisher allowfinaldraft |
| Permissão de Leitura | allow from all |
| Permissão de Atualização | não transferida |
| 5. Fontes relacionadas | |
| Vinculação | Trabalho não Vinculado à Tese/Dissertação |
| Repositório Espelho | iconet.com.br/banon/2006/11.26.21.31 |
| Unidades Imediatamente Superiores | 8JMKD3MGPCW/3EU29DP |
| Lista de Itens Citando | sid.inpe.br/bibdigital/2013/10.01.22.11 1 sid.inpe.br/mtc-m21/2012/07.13.14.45.47 1 |
| Divulgação | WEBSCI; PORTALCAPES; COMPENDEX; SCOPUS. |
| Acervo Hospedeiro | sid.inpe.br/mtc-m21b/2013/09.26.14.25.20 |
| 6. Notas | |
| Campos Vazios | alternatejournal archivist callnumber copyholder copyright creatorhistory descriptionlevel electronicmailaddress format isbn lineage mark nextedition notes orcid pages parameterlist parentrepositories previousedition previouslowerunit progress project rightsholder schedulinginformation secondarydate secondarykey secondarymark session shorttitle sponsor subject tertiarytype typeofwork url |
| 7. Controle da descrição | |
| e-Mail (login) | marciana |
| atualizar | |