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1. Identity statement
Reference TypeConference Paper (Conference Proceedings)
Sitemtc-m21c.sid.inpe.br
Holder Codeisadg {BR SPINPE} ibi 8JMKD3MGPCW/3DT298S
Identifier8JMKD3MGP3W34R/3SETPLP
Repositorysid.inpe.br/mtc-m21c/2018/12.27.12.44
Metadata Repositorysid.inpe.br/mtc-m21c/2018/12.27.12.44.29
Metadata Last Update2021:02.27.05.02.19 (UTC) administrator
Secondary KeyINPE--PRE/
Citation KeyRodríguezGómesEcheMagaMarq:2018:StSoWi
TitleA study of solar wind effects of Jupiter magnetosphere
Year2018
Access Date2024, May 16
Secondary TypePRE CN
2. Context
Author1 Rodríguez Gómes, Jenny Marcela
2 Echer, Ezequiel
3 Magalhães, Fabíola Pinho
4 Marques, M.
Resume Identifier1
2 8JMKD3MGP5W/3C9JH3D
Group1 GES-CEA-SESPG-INPE-MCTIC-GOV-BR
2 DIDGE-CGCEA-INPE-MCTIC-GOV-BR
3 GES-CEA-SESPG-INPE-MCTIC-GOV-BR
Affiliation1 Instituto Nacional de Pesquisas Espaciais (INPE)
2 Instituto Nacional de Pesquisas Espaciais (INPE)
3 Instituto Nacional de Pesquisas Espaciais (INPE)
4 Universidade Federal do Rio Grande do Norte (UFRN)
Author e-Mail Address1 jemfisi@gmail.com
2 ezequiel.echer@inpe.br
3 alisson.dallago@inpe.br
Conference NameSimpósio Brasileiro de Geofísica Espacial e Aeronomia, 7 (SBGEA)
Conference LocationSanta Maria, RS
Date05-09 nov
History (UTC)2018-12-27 12:44:29 :: simone -> administrator ::
2021-02-27 05:02:19 :: administrator -> simone :: 2018
3. Content and structure
Is the master or a copy?is the master
Content Stagecompleted
Transferable1
Content TypeExternal Contribution
Version Typepublisher
AbstractThe Sun drives many phenomena in the solar system. Its influence is mainly due to the magnetic phenomena. The solar wind interaction with the bodies of the solar system results in the formation of the magnetospheres. The Jupiter's magnetosphere in part is sensitive to the solar wind dynamic pressure variations. Several observations shown that aurora and radio emissions are intensified during higher solar wind pressure or induced by interplanetary shocks. Interplanetary shocks are driven by ICMEs or CIRS. The fast forward (FS) shock is mainly by ICMEs originated from CMEs. However, when CHs are evolving, fast streams emanate, and intercept the ambient solar wind. This interaction forms a compression region between the high speed stream and slow speed stream, it is limited by fast forward (FS) and fast reverse (RS) shocks. We present a study of fast forward and reverse shocks on the Jupiter magnetosphere. For this purpose, we use the propagated solar wind from Michigan Solar Wind model (mSWim) during the outbound period of the Cassini spacecraft. Also, the dynamic pressure will be obtained and analyzed. This work can contribute to understanding the complex Jupiter magnetosphere and its interaction with the solar wind.
AreaCEA
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4. Conditions of access and use
Languagept
User Groupsimone
Visibilityshown
Update Permissionnot transferred
5. Allied materials
Next Higher Units8JMKD3MGPCW/3EU29DP
8JMKD3MGPCW/3F2PBEE
Citing Item List
Host Collectionurlib.net/www/2017/11.22.19.04
6. Notes
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