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1. Identity statement
Reference TypeJournal Article
Sitemtc-m21c.sid.inpe.br
Holder Codeisadg {BR SPINPE} ibi 8JMKD3MGPCW/3DT298S
Identifier8JMKD3MGP3W34R/3TGF38E
Repositorysid.inpe.br/mtc-m21c/2019/06.21.00.02
Last Update2019:06.21.00.02.21 (UTC) administrator
Metadata Repositorysid.inpe.br/mtc-m21c/2019/06.21.00.02.21
Metadata Last Update2020:06.02.12.18.25 (UTC) administrator
DOI10.1029/2019GL082126
ISSN0094-8276
Citation KeyEcher:2019:InShPa
TitleInterplanetary shock parameters near Jupiter's orbit
Year2019
Access Date2024, May 17
Type of Workjournal article
Secondary TypePRE PI
Number of Files1
Size605 KiB
2. Context
AuthorEcher, Ezequiel
Resume Identifier8JMKD3MGP5W/3C9JH3D
GroupDIDGE-CGCEA-INPE-MCTIC-GOV-BR
AffiliationInstituto Nacional de Pesquisas Espaciais (INPE)
Author e-Mail Addressezequie.echer@inpe.br
JournalGeophysical Research Letters
Volume2019
Pages082126
Secondary MarkA1_INTERDISCIPLINAR A1_GEOGRAFIA A1_GEOCIÊNCIAS A1_ENGENHARIAS_III A1_ENGENHARIAS_I A1_CIÊNCIAS_AMBIENTAIS A1_CIÊNCIAS_AGRÁRIAS_I A1_BIODIVERSIDADE A2_QUÍMICA A2_ENGENHARIAS_IV A2_ENGENHARIAS_II A2_CIÊNCIAS_BIOLÓGICAS_I B1_ASTRONOMIA_/_FÍSICA B2_ENSINO
History (UTC)2019-06-21 00:02:21 :: simone -> administrator ::
2019-06-21 00:02:22 :: administrator -> simone :: 2019
2019-06-21 00:02:34 :: simone -> administrator :: 2019
2020-06-02 12:18:25 :: administrator -> simone :: 2019
3. Content and structure
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AbstractFast interplanetary shocks occurrence, their parameters, and drivers near Jupiter's orbit are determined in this paper. It was found that 70% of the fast shocks are forward (FS) and 30% are reverse (RS). Interplanetary coronal mass ejection‐driven FS occur more frequently in all solar cycle phases except in the declining phase, when corotating interaction region‐driven shocks predominate. Most of the shocks were quasi‐perpendicularly (65° to 70°) propagating relative to the ambient interplanetary magnetic field. The average shock magnetosonic Mach number is slightly higher for FS (2.6) than for RS (2.4), which in turn are stronger than shocks near 1 and 10 AU reported in previous works. This occurs because of the full development of corotating interaction region shocks and higher occurrence of strong interplanetary coronal mass ejections near 5 AU and that the magnetosonic speed at 5 AU has only 60% of its value at 1 AU.
AreaCEA
Arrangementurlib.net > BDMCI > Fonds > Produção anterior à 2021 > DIDGE > Interplanetary shock parameters...
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4. Conditions of access and use
data URLhttp://urlib.net/ibi/8JMKD3MGP3W34R/3TGF38E
zipped data URLhttp://urlib.net/zip/8JMKD3MGP3W34R/3TGF38E
Languageen
Target FileInterplanetary Shock Parameters Near Jupiter's Orbit.pdf
User Groupsimone
Visibilityshown
Archiving Policydenypublisher6 allowfinaldraft
Read Permissionallow from all
Update Permissionnot transferred
5. Allied materials
Next Higher Units8JMKD3MGPCW/3EU29DP
Citing Item Listsid.inpe.br/mtc-m21/2012/07.13.14.45.47 4
sid.inpe.br/bibdigital/2013/10.01.22.11 3
DisseminationWEBSCI; PORTALCAPES; AGU; COMPENDEX; SCOPUS.
Host Collectionurlib.net/www/2017/11.22.19.04
6. Notes
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