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1. Identity statement
Reference TypeJournal Article
Sitemtc-m16c.sid.inpe.br
Holder Codeisadg {BR SPINPE} ibi 8JMKD3MGPCW/3DT298S
Identifier8JMKD3MGP8W/35HFS8L
Repositorysid.inpe.br/mtc-m18@80/2009/06.25.16.33
Last Update2009:06.25.16.33.31 (UTC) administrator
Metadata Repositorysid.inpe.br/mtc-m18@80/2009/06.25.16.33.32
Metadata Last Update2020:04.28.17.48.42 (UTC) administrator
Secondary KeyINPE--PRE/
DOI10.1051/0004-6361/200811171
ISSN0004-6361
1432-0746
Citation KeyBorgazziLaraEcheAlve:2009:DyCoMa
TitleDynamics of coronal mass ejections in the interplanetary medium
Year2009
MonthMay
Access Date2024, May 17
Secondary TypePRE PI
Number of Files1
Size395 KiB
2. Context
Author1 Borgazzi, Andrea
2 Lara, A.
3 Echer, Ezequiel
4 Alves, Maria Virgínia
Resume Identifier1
2
3 8JMKD3MGP5W/3C9JH3D
Group1 DGE-CEA-INPE-MCT-BR
2
3 DGE-CEA-INPE-MCT-BR
4 LAP-CTE-INPE-MCT-BR
Affiliation1 Instituto Nacional de Pesquisas Espaciais (INPE)
2
3 Instituto Nacional de Pesquisas Espaciais (INPE)
4 Instituto Nacional de Pesquisas Espaciais (INPE)
JournalAstronomy & Astrophysics
Volume498
Number3
Pages885-889
History (UTC)2009-06-25 16:34:08 :: simone -> administrator ::
2020-04-28 17:48:42 :: administrator -> simone :: 2009
3. Content and structure
Is the master or a copy?is the master
Content Stagecompleted
Transferable1
Content TypeExternal Contribution
Keywordshydrodynamics
Sun: coronal mass ejections (CMEs)
interplanetary medium
AbstractContext. Coronal mass ejections (CMEs) are large plasma structures expelled from the low corona to the interplanetary space with a wide range of speeds. In the interplanetary medium CMEs suffer changes in their speeds because of interaction with the ambient solar wind. Aims. To understand the interplanetary CME (ICME) dynamics, we analyze the interaction between these structures and the ambient solar wind (SW), approaching the problem from the hydrodynamic point of view. Methods. We assume that the dynamics of the system is dominated by two kinds of drag-force dependence on speed (U), as similar to U and similar to U-2. Furthermore, we propose a model that takes variations of the ICME radius (R) and SW density (rho(sw)) into account as a function of the distance (x) as R(x) = x(0.78) and rho(sw)(x) = 1/x(2), respectively. Then, we solve the equation of motion and present exact solutions. Results. Considering CME speeds measured at a few solar radii and at one AU, we were able to constrain the values of the constants (viscosity and drag coefficient) for the linear (U) and quadratic (U-2) speed dependences, which seems to reproduce the ICME-SW system well. We found different solutions in which the concavity of the curves of the ICME speed profile changes, depending on the dominant factor, either the ICME radius or the SW density. Conclusions. This work shows that the macroscopic ICME propagation may be described by the hydrodynamic theory and that it is possible to find analytical solutions for the ICME-SW interaction.
AreaCEA
Arrangement 1urlib.net > BDMCI > Fonds > Produção anterior à 2021 > LABAP > Dynamics of coronal...
Arrangement 2urlib.net > BDMCI > Fonds > Produção anterior à 2021 > DIDGE > Dynamics of coronal...
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4. Conditions of access and use
data URLhttp://urlib.net/ibi/8JMKD3MGP8W/35HFS8L
zipped data URLhttp://urlib.net/zip/8JMKD3MGP8W/35HFS8L
Languageen
Target FileA9RE.tmp.pdf
User Groupadministrator
simone
Visibilityshown
Archiving Policyallowpublisher allowfinaldraft
Read Permissionallow from all
5. Allied materials
Mirror Repositorysid.inpe.br/mtc-m18@80/2008/03.17.15.17.24
Next Higher Units8JMKD3MGPCW/3ET2RFS
8JMKD3MGPCW/3EU29DP
Citing Item Listsid.inpe.br/mtc-m21/2012/07.13.14.45.47 2
sid.inpe.br/bibdigital/2013/10.01.22.11 1
sid.inpe.br/bibdigital/2013/09.25.21.49 1
Host Collectionsid.inpe.br/mtc-m18@80/2008/03.17.15.17
6. Notes
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