Close
Metadata

Identity statement area
Reference TypeJournal Article
Sitemtc-m16d.sid.inpe.br
Holder Codeisadg {BR SPINPE} ibi 8JMKD3MGPCW/3DT298S
Identifier8JMKD3MGP7W/37JT9U2
Repositorysid.inpe.br/mtc-m19@80/2010/06.01.14.06   (restricted access)
Last Update2010:06.01.14.06.27 (UTC) administrator
Metadatasid.inpe.br/mtc-m19@80/2010/06.01.14.06.29
Metadata Last Update2021:07.18.04.02.29 (UTC) administrator
Secondary KeyINPE--PRE/
DOI10.1016/j.jastp.2010.04.003
ISSN1364-6826
Citation KeyTsurutaniEcheGuarGonz:2011:PrTwSo
TitleThe properties of two solar wind high speed streams and related geomagnetic activity during the declining phase of solar cycle 23
Year2011
MonthJan.
Access Date2021, July 25
Number of Files1
Size2175 KiB
Context area
Author1 Tsurutani, Bruce T.
2 Echer, Ezequiel
3 Guarnieri, Fernando L.
4 Gonzalez Alarcon, Walter Demétrio
Resume Identifier1
2 8JMKD3MGP5W/3C9JH3D
3
4 8JMKD3MGP5W/3C9JJC4
Group1
2 DGE-CEA-INPE-MCT-BR
3
4 DAS-CEA-INPE-MCT-BR
Affiliation1 CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA
2 Instituto Nacional de Pesquisas Espaciais (INPE)
3 Universidade do Vale do Paraiba (UNIVAP)
4 Instituto Nacional de Pesquisas Espaciais (INPE)
JournalJournal of Atmospheric and Solar-Terrestrial Physics
Volume73
Number1
Pages164-177
Secondary TypePRE PI
Secondary MarkB2_ASTRONOMIA_/_FÍSICA B1_CIÊNCIAS_BIOLÓGICAS_I B1_ECOLOGIA_E_MEIO_AMBIENTE B1_ENGENHARIAS_IV B1_GEOCIÊNCIAS A2_INTERDISCIPLINAR
History (UTC)2010-07-05 14:54:45 :: simone -> marciana :: 2010
2011-02-23 13:14:59 :: marciana :: 2010 -> 2011
2011-08-04 14:46:51 :: marciana -> administrator :: 2011
2011-11-07 05:50:29 :: administrator -> marciana :: 2011
2011-11-10 13:00:38 :: marciana -> administrator :: 2011
2021-07-18 04:02:29 :: administrator -> tereza@sid.inpe.br :: 2011
Content and structure area
Is the master or a copy?is the master
Content Stagecompleted
Transferable1
Content TypeExternal Contribution
Version Typepublisher
KeywordsHigh speed solar wind streams, Interplanetary Alfvenicity, Geomagnetic activity, HILDCAAs.
AbstractTwo high speed stream (HSS) solar wind intervals (days 283¨C294 and 314¨C318, 2003, hereafter called Events 1 and 2) during the declining phase of solar cycle 23 have been examined in detail for their interplanetary characteristics and their resultant geomagnetic activity. Event 1 had an associated storm initial phase with peak Dst=+9 nT. This was caused by a high plasma density heliospheric plasma sheet (HPS) which impacted the magnetosphere. The southward component of IMF Bz fluctuations in the corotating interaction regions (CIRs) of both Events 1 and 2 led to peak storm main phases of Dst=−85 and −62 nT, respectively. The extended storm ¡°recovery¡± phases were associated with ¦¤B/Bo 1¨C2 Alfv¨¦nic fluctuations in the HSS proper. High-intensity, long-duration, continuous AE (HILDCAA) intervals were present, presumably due to the southward component of the Alfv¨¦n waves. The IMF Bx¨CVx 4-h cross-correlation values were >0.8 in Event 2, and lower, >0.6, in Event 1. The difference in Alfv¨¦nicity between the two HSS events is not understood at present. The IMF Bz 10-min to 3-h variances and are highest during the CIRs. The normalized variances during the HSS proper are approximately the same as those for the CIRs. For Event 1, the 1-h IMF and are 5.0 nT2 and 1.1¡Á10−1, respectively. The IMF Bz-AE cross-correlation (c.c.) coefficients during the storm main phase of Event 1 and for 24-h of the HSS of Event 2 give similar results. For the Event 1, a peak c.c. of −0.4 occurred with a lag of 103 min, and for Event 2 a peak c.c of −0.38 with a lag of 67 min was obtained. Both c.c. results were sharply peaked. The decay-portion of a HSS prior to Event 1 was characterized by low Np, low Bo and low Alfv¨¦n wave amplitudes. The 1-h IMF and were 0.84 nT2 and 2.9¡Á10−2, respectively. This quiet interplanetary interval led to a quiet geomagnetic activity period (AE<100 nT, Dst +5 nT). On the other hand, what is quite surprising is that this region was the most purely ¡°Alfv¨¦nic¡± interval studied (c.c. of Bx-Vx=0.95).The ¦Å parameter was calculated using both GSE and GSM coordinates. It was found that ¦Å is 30% larger for GSM coordinates. Thus, the major cause of geomagnetic activity during HSSs is the large amplitude Alfv¨¦n waves but not coordinate transformations. Sector polarities (IMF By values) may be a secondary factor. However, other models, like the tilted solar dipole, should be considered as well.
AreaCEA
Arrangement 1urlib.net > BDMCI > Fonds > Produção > DIDAS > The properties of...
Arrangement 2urlib.net > BDMCI > Fonds > Produção > DIDGE > The properties of...
source Directory Contentthere are no files
agreement Directory Contentthere are no files
Conditions of access and use area
Languageen
Target Filethe properties of two solar.pdf
User Groupadministrator
marciana
simone
Visibilityshown
Archiving Policydenypublisher denyfinaldraft24
Read Permissiondeny from all and allow from 150.163
Update Permissionnot transferred
Allied materials area
Mirror Repositorysid.inpe.br/mtc-m19@80/2009/08.21.17.02.53
Next Higher Units8JMKD3MGPCW/3ETR8EH
8JMKD3MGPCW/3EU29DP
DisseminationWEBSCI; PORTALCAPES; AGU; MGA; COMPENDEX.
Host Collectionsid.inpe.br/mtc-m19@80/2009/08.21.17.02
Notes area
Empty Fieldsalternatejournal archivist callnumber copyholder copyright creatorhistory descriptionlevel e-mailaddress electronicmailaddress format isbn label lineage mark nextedition notes orcid parameterlist parentrepositories previousedition previouslowerunit progress project readergroup rightsholder secondarydate session shorttitle sponsor subject tertiarymark tertiarytype typeofwork url
Description control area
e-Mail (login)tereza@sid.inpe.br
update 

Close