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1. Identity statement
Reference TypeJournal Article
Sitemtc-m21c.sid.inpe.br
Holder Codeisadg {BR SPINPE} ibi 8JMKD3MGPCW/3DT298S
Identifier8JMKD3MGP3W34R/3S4SLLP
Repositorysid.inpe.br/mtc-m21c/2018/10.26.18.26
Last Update2018:10.26.18.26.45 (UTC) simone
Metadata Repositorysid.inpe.br/mtc-m21c/2018/10.26.18.26.45
Metadata Last Update2021:07.28.23.02.28 (UTC) administrator
DOI10.1051/0004-6361/201833586
ISSN0004-6361
1432-0746
Citation KeyZarkaMaLoRyLaEcCe:2018:JuRaEm
TitleJupiter radio emission induced by Ganymede and consequences for the radio detection of exoplanets
Year2018
MonthOct.
Access Date2024, May 17
Type of Workjournal article
Secondary TypePRE PI
Number of Files1
Size4540 KiB
2. Context
Author1 Zarka, P.
2 Marques, M. S.
3 Louis, C.
4 Ryabov, V. B.
5 Lamy, L.
6 Echer, Ezequiel
7 Cecconi, B.
Resume Identifier1
2
3
4
5
6 8JMKD3MGP5W/3C9JH3D
Group1
2
3
4
5
6 DIDGE-CGCEA-INPE-MCTIC-GOV-BR
Affiliation1 LESIA, Observatoire de Paris
2 LESIA, Observatoire de Paris
3 LESIA, Observatoire de Paris
4 Future University Hakodate
5 LESIA, Observatoire de Paris
6 Instituto Nacional de Pesquisas Espaciais (INPE)
7 LESIA, Observatoire de Paris
Author e-Mail Address1
2
3
4
5
6 ezequiel.echer@inpe.br
JournalAstronomy & Astrophysics
Volume618
NumberA84
Secondary MarkA1_GEOCIÊNCIAS A1_ENGENHARIAS_III A2_MATEMÁTICA_/_PROBABILIDADE_E_ESTATÍSTICA A2_INTERDISCIPLINAR A2_ENGENHARIAS_IV A2_ASTRONOMIA_/_FÍSICA B2_ENSINO C_ENGENHARIAS_II
History (UTC)2018-10-26 18:26:45 :: simone -> administrator ::
2018-10-26 18:26:46 :: administrator -> simone :: 2018
2018-10-26 18:27:20 :: simone -> administrator :: 2018
2021-07-28 23:02:28 :: administrator -> simone :: 2018
3. Content and structure
Is the master or a copy?is the master
Content Stagecompleted
Transferable1
Content TypeExternal Contribution
Version Typepublisher
Keywordsradio continuum: planetary systems
plasmas
magnetic fields
planet-star interactions
planets and satellites: individuals: Jupiter
Ganymede
Io
catalogs
AbstractBy analysing a database of 26 yr of observations of Jupiter with the Nancay Decameter Array, we unambiguously identify the radio emissions caused by the Ganymede-Jupiter interaction. We study the energetics of these emissions via the distributions of their intensities, duration, and power, and compare them to the energetics of the Io-Jupiter radio emissions. This allows us to demonstrate that the average emitted radio power is proportional to the Poynting flux from the rotating Jupiter's magnetosphere intercepted by the obstacle. We then generalize this result to the radio-magnetic scaling law that appears to apply to all plasma interactions between a magnetized flow and an obstacle, magnetized or not. Extrapolating this scaling law to the parameter range corresponding to hot Jupiters, we predict large radio powers emitted by these objects, that should result in detectable radio flux with new-generation radiotelescopes. Comparing the distributions of the durations of Ganymede-Jupiter and Io-Jupiter emission events also suggests that while the latter results from quasi-permanent Alfven wave excitation by Io, the former likely results from sporadic reconnection between magnetic fields Ganymede and Jupiter, controlled by Jupiter's magnetic field geometry and modulated by its rotation.
AreaCEA
Arrangementurlib.net > BDMCI > Fonds > Produção anterior à 2021 > DIDGE > Jupiter radio emission...
doc Directory Contentaccess
source Directory Contentthere are no files
agreement Directory Content
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4. Conditions of access and use
data URLhttp://urlib.net/ibi/8JMKD3MGP3W34R/3S4SLLP
zipped data URLhttp://urlib.net/zip/8JMKD3MGP3W34R/3S4SLLP
Languageen
Target Filezarka_jupiter.pdf
User Groupsimone
Reader Groupadministrator
simone
Visibilityshown
Archiving Policyallowpublisher allowfinaldraft
Update Permissionnot transferred
5. Allied materials
Next Higher Units8JMKD3MGPCW/3EU29DP
Citing Item Listsid.inpe.br/mtc-m21/2012/07.13.14.45.47 9
sid.inpe.br/bibdigital/2013/10.01.22.11 1
DisseminationWEBSCI; PORTALCAPES; COMPENDEX; SCOPUS.
Host Collectionurlib.net/www/2017/11.22.19.04
6. Notes
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