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1. Identity statement
Reference TypeJournal Article
Sitemtc-m16d.sid.inpe.br
Holder Codeisadg {BR SPINPE} ibi 8JMKD3MGPCW/3DT298S
Identifier8JMKD3MGP7W/3B58HBB
Repositorysid.inpe.br/mtc-m19/2012/01.02.15.51   (restricted access)
Last Update2012:06.26.12.36.23 (UTC) secretaria.cpa@dir.inpe.br
Metadata Repositorysid.inpe.br/mtc-m19/2012/01.02.15.51.14
Metadata Last Update2021:07.18.04.02.15 (UTC) administrator
Secondary KeyINPE--PRE/
DOI10.1016/j.jastp.2011.09.001
ISSN1364-6826
Citation KeyCerratoSaiCidGonPal:2012:SoInTr
TitleSolar and interplanetary triggers of the largest DST variations during solar cycle 23
Year2012
MonthMay
Access Date2023, Jan. 31
Secondary TypePRE PI
Number of Files1
Size2126 KiB
2. Context
Author1 Cerrato, Yolanda
2 Saiz, E.
3 Cid, Consuelo
4 Gonzalez, Walter Demetrio
5 Palacios, J.
Resume Identifier1
2
3
4 8JMKD3MGP5W/3C9JJC4
Group1 DGE-CEA-INPE-MCTI-GOV-BR
2
3 DGE-CEA-INPE-MCTI-GOV-BR
4 DGE-CEA-INPE-MCTI-GOV-BR
Affiliation1 Instituto Nacional de Pesquisas Espaciais (INPE)
2
3 Instituto Nacional de Pesquisas Espaciais (INPE)
4 Instituto Nacional de Pesquisas Espaciais (INPE)
e-Mail Addresssecretaria.cpa@dir.inpe.br
JournalJournal of Atmospheric and Solar-Terrestrial Physics
Volume80
Pages111-123
Secondary MarkB2_ASTRONOMIA_/_FÍSICA B1_CIÊNCIAS_BIOLÓGICAS_I B1_ECOLOGIA_E_MEIO_AMBIENTE B1_ENGENHARIAS_IV B1_GEOCIÊNCIAS A2_INTERDISCIPLINAR
History (UTC)2012-01-02 15:51:14 :: secretaria.cpa@dir.inpe.br -> administrator ::
2012-01-02 15:51:14 :: administrator -> secretaria.cpa@dir.inpe.br :: 2011
2012-06-26 12:36:23 :: secretaria.cpa@dir.inpe.br :: 2011 -> 2012
2012-06-26 12:36:34 :: secretaria.cpa@dir.inpe.br -> administrator :: 2012
2012-11-16 17:03:30 :: administrator -> secretaria.cpa@dir.inpe.br :: 2012
2012-12-11 16:55:54 :: secretaria.cpa@dir.inpe.br -> administrator :: 2012
2021-07-18 04:02:15 :: administrator -> marciana :: 2012
3. Content and structure
Is the master or a copy?is the master
Content Stagecompleted
Transferable1
Content TypeExternal Contribution
Version Typepublisher
KeywordsDst index
Geomagnetic storm
Halo CME
Interplanetary disturbances
AbstractWe present the results of an investigation from the Sun to the Earth of the sequence of events that caused major Dst decreases (¦¤Dst¡(C100 nT during 1 h) that occurred during 1996¨C2005. These events are expected to be better related to geomagnetic induced current (GIC) events than those events where any geomagnetic index is far from its quiet time value. At least one full halo CME with a speed on the plane of sky above 900 km/s participates in every studied event. The seven events were triggered by interplanetary signatures, which arise as a consequence of interaction among different solar ejections. The interaction arises at different stages from the solar surface, between segments of a filament, to the interplanetary medium, appearing as ejecta or multiple-magnetic clouds (MultiMCs). In other cases, shock waves overtake or compress previous ICMEs and at other times the interaction also appears between magnetic clouds (MCs) and streams.
AreaCEA
Arrangementurlib.net > BDMCI > Fonds > Produção > DIDGE > Solar and interplanetary...
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Mirror Repositorysid.inpe.br/mtc-m19@80/2009/08.21.17.02.53
Next Higher Units8JMKD3MGPCW/3EU29DP
DisseminationWEBSCI; PORTALCAPES; AGU; MGA; COMPENDEX.
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6. Notes
Empty Fieldsalternatejournal archivist callnumber copyholder copyright creatorhistory descriptionlevel electronicmailaddress format isbn label lineage mark nextedition notes number orcid parameterlist parentrepositories previousedition previouslowerunit progress project rightsholder secondarydate session shorttitle sponsor subject targetfile tertiarymark tertiarytype typeofwork url
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1. Identity statement
Reference TypeJournal Article
Sitemtc-m16d.sid.inpe.br
Holder Codeisadg {BR SPINPE} ibi 8JMKD3MGPCW/3DT298S
Identifier8JMKD3MGP7W/3D7BCQL
Repositorysid.inpe.br/mtc-m19/2012/12.12.18.12
Last Update2013:01.24.13.35.05 (UTC) administrator
Metadata Repositorysid.inpe.br/mtc-m19/2012/12.12.18.12.48
Metadata Last Update2018:06.05.04.13.29 (UTC) administrator
Secondary KeyINPE--PRE/
DOI10.5194/angeo-30-1515-2012
ISSN0992-7689
Citation KeyTreumannBaumGonz:2012:MaFiLi
TitleCollisionless reconnection: Magnetic field line interaction
Year2012
Access Date2023, Jan. 31
Secondary TypePRE PI
Number of Files1
Size1587 KiB
2. Context
Author1 Treumann, R. A.
2 Baumjohann, W.
3 Gonzalez, W. D.
Group1
2
3 DGE-CEA-INPE-MCTI-GOV-BR
Affiliation1
2
3 Instituto Nacional de Pesquisas Espaciais (INPE)
e-Mail Addressmarcelo.pazos@inpe.br
JournalAnnales Geophysicae
Volume30
Pages1515-1528
History (UTC)2013-01-24 13:35:05 :: marcelo.pazos@sid.inpe.br -> administrator :: 2012
2018-06-05 04:13:29 :: administrator -> marcelo.pazos@inpe.br :: 2012
3. Content and structure
Is the master or a copy?is the master
Content Stagecompleted
Transferable1
Content TypeExternal Contribution
AbstractMagnetic field lines are quantum objects carrying one quantum Fi0 = 2 Pi h/e of magnetic flux and have finite radius m. Here we argue that they possess a very specific dynamical interaction. Parallel field lines reject each other. When confined to a certain area they form two-dimensional lattices of hexagonal structure. We estimate the filling factor of such an area. Anti-parallel field lines, on the other hand, attract each other.We identify the physical mechanism as being due to the action of the gauge potential field, which we determine quantum mechanically for two parallel and two antiparallel field lines. The distortion of the quantum electrodynamic vacuum causes a cloud of virtual pairs. We calculate the virtual pair production rate from quantum electrodynamics and estimate the virtual pair cloud density, pair current and Lorentz force density acting on the field lines via the pair cloud. These properties of field line dynamics become important in collisionless reconnection, consistently explaining why and how reconnection can spontaneously set on in the field-free centre of a current sheet below the electron-inertial scale.
AreaCEA
ArrangementCollisionless reconnection: Magnetic...
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data URLhttp://urlib.net/ibi/8JMKD3MGP7W/3D7BCQL
zipped data URLhttp://urlib.net/zip/8JMKD3MGP7W/3D7BCQL
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Mirror Repositorysid.inpe.br/mtc-m19@80/2009/08.21.17.02.53
Next Higher Units8JMKD3MGPCW/3EU29DP
URL (untrusted data)www.ann-geophys.net/30/1515/2012/
DisseminationWEBSCI; PORTALCAPES; MGA; COMPENDEX.
Host Collectionsid.inpe.br/mtc-m19@80/2009/08.21.17.02
6. Notes
Empty Fieldsalternatejournal archivist callnumber copyholder copyright creatorhistory descriptionlevel electronicmailaddress format isbn keywords label language lineage mark month nextedition notes number orcid parameterlist parentrepositories previousedition previouslowerunit progress project resumeid rightsholder secondarydate secondarymark session shorttitle sponsor subject targetfile tertiarymark tertiarytype typeofwork versiontype
7. Description control
e-Mail (login)marcelo.pazos@inpe.br
update 

1. Identity statement
Reference TypeJournal Article
Sitemtc-m16d.sid.inpe.br
Holder Codeisadg {BR SPINPE} ibi 8JMKD3MGPCW/3DT298S
Identifier8JMKD3MGP7W/3D774TP
Repositorysid.inpe.br/mtc-m19/2012/12.11.18.44
Last Update2013:01.23.16.28.05 (UTC) administrator
Metadata Repositorysid.inpe.br/mtc-m19/2012/12.11.18.44.56
Metadata Last Update2018:06.05.04.13.28 (UTC) administrator
Secondary KeyINPE--PRE/
ISSN0367-8393
0975-105X
Citation KeyKane:2012:CoRaFo
TitleCosmic ray Forbush decreases after the giant solar flare of 15 February 2011
ProjectNational Science Foundation, USA (grants ANT-0739620 and ANT-0838839); FINEP-537/CT
Year2012
Access Date2023, Jan. 31
Secondary TypePRE PI
Number of Files1
Size74 KiB
2. Context
AuthorKane, Rajaram Purushottam
Resume IdentifierHREF="http://urlib.net/8JMKD3MGP5W/3C9JJ4U">8JMKD3MGP5W/3C9JJ4U
GroupDGE-CEA-INPE-MCTI-GOV-BR
AffiliationInstituto Nacional de Pesquisas Espaciais (INPE)
Author e-Mail Addresskane@dge.inpe.br
e-Mail Addressmarcelo.pazos@inpe.br
JournalIndian Journal of Radio and Space Physics
Volume41
NumberOct.
Pages520-523
History (UTC)2013-01-16 17:49:17 :: marcelo.pazos@sid.inpe.br -> administrator :: 2012
2013-01-20 15:47:53 :: administrator -> marcelo.pazos@sid.inpe.br :: 2012
2013-01-23 16:28:05 :: marcelo.pazos@sid.inpe.br -> administrator :: 2012
2013-01-30 18:15:50 :: administrator -> banon :: 2012
2013-02-04 17:53:13 :: banon -> administrator :: 2012
2018-06-05 04:13:28 :: administrator -> marcelo.pazos@inpe.br :: 2012
3. Content and structure
Is the master or a copy?is the master
Content Stagecompleted
Transferable1
Content TypeExternal Contribution
KeywordsForbush decrease
solar flare
Coronal Mass Ejection (CME)
geomagnetic storm
cosmic ray
AbstractA very strong X-ray solar flare occurred at about 0200 hrs UT on 15 February 2011. It was associated with a coronal mass ejection (CME) but the CME was not very strong and its interplanetary CME (ICME) took about 70 h to reach the Earth. Also, the ICME blob had a moderate, short-lived magnetic field B, so the resulting cosmic ray Forbush decrease (FD) was weak. The Bz component was only slightly negative, so the resulting geomagnetic storm magnitude Dst was negligibly small. Thus, this giant solar flare had very poor geo-effectiveness indicating that large flares need not necessarily lead to significant storm effects on Earth, particularly in the early part of a sunspot cycle when overall solar activity would be weak.
AreaCEA
Arrangementurlib.net > BDMCI > Fonds > Produção anterior à 2021 > DIDGE > Cosmic ray Forbush...
doc Directory Contentaccess
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4. Conditions of access and use
data URLhttp://urlib.net/ibi/8JMKD3MGP7W/3D774TP
zipped data URLhttp://urlib.net/zip/8JMKD3MGP7W/3D774TP
Languageen
User Groupadministrator
banon
marcelo.pazos@inpe.br
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Update Permissionnot transferred
5. Allied materials
Mirror Repositorysid.inpe.br/mtc-m19@80/2009/08.21.17.02.53
Next Higher Units8JMKD3MGPCW/3EU29DP
DisseminationWEBSCI; PORTALCAPES.
Host Collectionsid.inpe.br/mtc-m19@80/2009/08.21.17.02
6. Notes
Empty Fieldsalternatejournal archivist callnumber copyholder copyright creatorhistory descriptionlevel doi format isbn label lineage mark month nextedition notes orcid parameterlist parentrepositories previousedition previouslowerunit progress readpermission rightsholder secondarydate secondarymark session shorttitle sponsor subject targetfile tertiarymark tertiarytype typeofwork url versiontype
7. Description control
e-Mail (login)marcelo.pazos@inpe.br
update 

1. Identity statement
Reference TypeJournal Article
Sitemtc-m16d.sid.inpe.br
Holder Codeisadg {BR SPINPE} ibi 8JMKD3MGPCW/3DT298S
Identifier8JMKD3MGP7W/3D5QSNB
Repositorysid.inpe.br/mtc-m19/2012/12.03.12.51   (restricted access)
Last Update2013:01.23.11.39.29 (UTC) administrator
Metadata Repositorysid.inpe.br/mtc-m19/2012/12.03.12.51.18
Metadata Last Update2018:06.05.04.13.15 (UTC) administrator
Secondary KeyINPE--PRE/
DOI10.1016/j.chaos.2012.06.004
ISSN0960-0779
Citation KeyChagasTolRemChiVal:2012:OpFeCo
TitleOptimal feedback control of the forced van der Pol system
ProjectFondecyt Grant 1110135 (Chile)
Year2012
Access Date2023, Jan. 31
Secondary TypePRE PI
Number of Files1
Size922 KiB
2. Context
Author1 Chagas, T. P.
2 Toledo, B. A.
3 Rempel, E. L.
4 Chian, A. C. -L.
5 Valdivia, J. A.
Group1
2
3
4 DGE-CEA-INPE-MCTI-GOV-BR
Affiliation1 Santa Cruz State University (UESC), 45662-900 Ilhéus-BA, Brazil
2 Institut of Aeronautical Technology (ITA), 12228-900 São José dos Campos-SP, Brazil
3 Institut of Aeronautical Technology (ITA), 12228-900 São José dos Campos-SP, Brazil
4 Instituto Nacional de Pesquisas Espaciais (INPE)
5 Departamento de Física, Facultad de Ciencias, Universidad de Chile, Casilla 653, Santiago, Chile
JournalChaos, Solitons and Fractals
Volume45
Number9-10
Pages1147-1156
History (UTC)2013-01-23 11:39:29 :: marciana -> administrator :: 2012
2018-06-05 04:13:15 :: administrator -> marciana :: 2012
3. Content and structure
Is the master or a copy?is the master
Content Stagecompleted
Transferable1
Content TypeExternal Contribution
Version Typepublisher
Keywordschaos control
characteristic multiplier
control effort
delay differential equations
delayed feedback control
DFC method
feedback control strategies
floquet multiplier
forcing amplitudes
optimal control gain
optimal feedback control
optimization problems
phase spaces
proportional feedback
steady state errors
unstable periodic orbits
Van Der Pol systems
AbstractA simple feedback control strategy for chaotic systems is investigated using the forced van der Pol system as an example. The strategy regards chaos control as an optimization problem, where the maximum magnitude Floquet multiplier of a target unstable periodic orbit (UPO) is used as a cost function that needs to be minimized. Thus, the method obtains the optimal control gain in terms of the stability of the target UPO. This strategy was recently proposed for the proportional feedback control (PFC) method. Here, it is extended to the highly popular delayed feedback control (DFC) method. Since the DFC method treats the system as a delay-differential equation whose phase space is infinite-dimensional, the characteristic multipliers are found through a truncation in the number of delayed states. Control of a target UPO is achieved for several values of the forcing amplitude. We compare the DFC and PFC methods in terms of stability of the controlled orbit, steady state error and control effort.
AreaCEA
Arrangementurlib.net > BDMCI > Fonds > Produção anterior à 2021 > DIDGE > Optimal feedback control...
doc Directory Contentaccess
source Directory Contentthere are no files
agreement Directory Content
agreement.html 03/12/2012 10:51 1.0 KiB 
4. Conditions of access and use
Languageen
User Groupadministrator
marciana
Reader Groupadministrator
marciana
Visibilityshown
Archiving Policydenypublisher denyfinaldraft24
Read Permissiondeny from all and allow from 150.163
Update Permissionnot transferred
5. Allied materials
Mirror Repositorysid.inpe.br/mtc-m19@80/2009/08.21.17.02.53
Next Higher Units8JMKD3MGPCW/3EU29DP
DisseminationWEBSCI
Host Collectionsid.inpe.br/mtc-m19@80/2009/08.21.17.02
6. Notes
Empty Fieldsalternatejournal archivist callnumber copyholder copyright creatorhistory descriptionlevel e-mailaddress electronicmailaddress format isbn label lineage mark month nextedition notes orcid parameterlist parentrepositories previousedition previouslowerunit progress resumeid rightsholder secondarydate secondarymark session shorttitle sponsor subject targetfile tertiarymark tertiarytype typeofwork url
7. Description control
e-Mail (login)marciana
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1. Identity statement
Reference TypeJournal Article
Sitemtc-m16d.sid.inpe.br
Holder Codeisadg {BR SPINPE} ibi 8JMKD3MGPCW/3DT298S
Identifier8JMKD3MGP7W/3D5CK3P
Repositorysid.inpe.br/mtc-m19/2012/11.30.17.41
Last Update2013:07.31.11.50.43 (UTC) administrator
Metadata Repositorysid.inpe.br/mtc-m19/2012/11.30.17.41.35
Metadata Last Update2018:06.05.04.13.15 (UTC) administrator
Secondary KeyINPE--PRE/
DOI10.1051/0004-6361/201219454
ISSN0004-6361
1432-0746
Citation KeyZimovetsVilChiShaStr:2012:SpReOb
TitleSpatially resolved observations of a split-band coronal type II radio burst
Year2012
Access Date2023, Jan. 31
Secondary TypePRE PI
Number of Files1
Size2957 KiB
2. Context
Author1 Zimovets, I.
2 Vilmer, N.
3 Chian, Abraham Chian Long
4 Sharykin, I.
5 Struminsky, A.
Group1
2
3 DGE-CEA-INPE-MCTI-GOV-BR
Affiliation1 Space Research Institute (IKI) of RAS, Moscow, Russian Federation
2 LESIA, Observatoire de Paris, CNRS, UPMC, Université Paris-Diderot, 5 place Jules Janssen, 92195 Meudon cedex, France
3 Instituto Nacional de Pesquisas Espaciais (INPE)
4 Moscow Institute of Physics and Technology, State University, Institutskii per. 9, Dolgoprudny, 141700 Moscow Region, Russian Federation
5 Moscow Institute of Physics and Technology, State University, Institutskii per. 9, Dolgoprudny, 141700 Moscow Region, Russian Federation
Author e-Mail Address1 ivanzim@iki.rssi.ru
2
3 achian@dge.inpe.br
JournalAstronomy & Astrophysics
Volume547
NumberA6
Secondary MarkA2_ASTRONOMIA_/_FÍSICA A1_ENGENHARIAS_II B1_ENGENHARIAS_IV B5_ENSINO_DE_CIÊNCIAS_E_MATEMATICA A1_GEOCIÊNCIAS A2_MATEMÁTICA_/_PROBABILIDADE_E_ESTATÍSTICA
History (UTC)2012-12-05 13:10:41 :: marciana -> administrator :: 2012
2012-12-10 18:44:19 :: administrator -> marciana :: 2012
2013-01-20 15:22:56 :: marciana -> administrator :: 2012
2018-06-05 04:13:15 :: administrator -> marciana :: 2012
3. Content and structure
Is the master or a copy?is the master
Content Stagecompleted
Transferable1
Content TypeExternal Contribution
Version Typepublisher
Keywordscorona
flares
sun radiation
X-rays
gamma rays
active regions
band splitting
blast shock wave
downstream region
Eruptive events
hard X ray
high energy
high frequency components
impulsive phase
AbstractThe origin of coronal type II radio bursts and the nature of their band splitting are still not fully understood, though a number of scenarios have been proposed to explain them. This is largely due to the lack of detailed spatially resolved observations of type II burst sources and of their relations to magnetoplasma structure dynamics in parental active regions. To make progress in solving this problem on the basis of one extremely well observed solar eruptive event. The relative dynamics of multithermal eruptive plasmas, observed in detail by the Atmospheric Imaging Assembly onboard the Solar Dynamics Observatory, and of harmonic type II burst sources, observed by the Nançay Radioheliograph at ten frequencies from 445 to 151 MHz, was studied for the 3 November 2010 event arising from an active region behind the east solar limb. Special attention was given to the band splitting of the burst. Analysis was supplemented by investigation of coronal hard X-ray (HXR) sources observed by the Reuven Ramaty High-Energy Solar Spectroscopic Imager. We found that the flare impulsive phase was accompanied by the formation of a double coronal HXR source, whose upper part coincided with the hot (T ≈ 10 MK) eruptive plasma blob. The leading edge (LE) of the eruptive plasmas (T ≈ 1-2 MK) moved upward from the flare region with a speed of v ≈ 900-1400 km s -1. The type II burst source initially appeared just above the LE apex and moved with the same speed and in the same direction. After ≈ 20 s, it started to move about twice as fast, but still in the same direction. At any given moment, the low-frequency component (LFC) source of the splitted type II burst was situated above the high-frequency component (HFC) source, which in turn was situated above the LE. We also found that at a given frequency the HFC source was located slightly closer to the photosphere than the LFC source. Based on the set of established observational facts, we conclude that the shock wave, which could be responsible for the observed type II radio burst, was initially driven by the multi-temperature eruptive plasmas, but later transformed to a freely propagating blast shock wave. The preferable interpretation of the type II burst splitting is that its LFC was emitted from the upstream region of the shock, whereas the HFC was emitted from the downstream region. The shock wave in this case could be subcritical.
AreaCEA
Arrangementurlib.net > BDMCI > Fonds > Produção anterior à 2021 > DIDGE > Spatially resolved observations...
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data URLhttp://urlib.net/ibi/8JMKD3MGP7W/3D5CK3P
zipped data URLhttp://urlib.net/zip/8JMKD3MGP7W/3D5CK3P
Languageen
Target File1208.5267v1.pdf
User Groupadministrator
marciana
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Archiving Policyallowpublisher allowfinaldraft
Read Permissionallow from all
Update Permissionnot transferred
5. Allied materials
Mirror Repositorysid.inpe.br/mtc-m19@80/2009/08.21.17.02.53
Next Higher Units8JMKD3MGPCW/3EU29DP
DisseminationWEBSCI; PORTALCAPES; MGA; COMPENDEX.
Host Collectionsid.inpe.br/mtc-m19@80/2009/08.21.17.02
6. Notes
Empty Fieldsalternatejournal archivist callnumber copyholder copyright creatorhistory descriptionlevel e-mailaddress format isbn label lineage mark month nextedition notes orcid pages parameterlist parentrepositories previousedition previouslowerunit progress project resumeid rightsholder secondarydate session shorttitle sponsor subject tertiarymark tertiarytype typeofwork url
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1. Identity statement
Reference TypeJournal Article
Sitemtc-m16d.sid.inpe.br
Holder Codeisadg {BR SPINPE} ibi 8JMKD3MGPCW/3DT298S
Identifier8JMKD3MGP7W/3CHCR4H
Repositorysid.inpe.br/mtc-m19/2012/08.30.12.34   (restricted access)
Last Update2012:08.30.18.37.47 (UTC) administrator
Metadata Repositorysid.inpe.br/mtc-m19/2012/08.30.12.34.27
Metadata Last Update2018:06.05.04.12.55 (UTC) administrator
Secondary KeyINPE--PRE/
DOI10.1016/j.pss.2011.12.011
ISSN0032-0633
Citation KeyKane:2012:InGePa
TitleInterplanetary and geomagnetic parameters during January 16-26, 2005
ProjectFINEP-537/CT
Year2012
MonthMarch
Access Date2023, Jan. 31
Secondary TypePRE PI
Number of Files1
Size214 KiB
2. Context
AuthorKane, Rajaram Purushottam
Resume IdentifierHREF="http://urlib.net/8JMKD3MGP5W/3C9JJ4U">8JMKD3MGP5W/3C9JJ4U
GroupDGE-CEA-INPE-MCTI-GOV-BR
AffiliationInstituto Nacional de Pesquisas Espaciais (INPE)
JournalPlanetary and Space Science
Volume62
Number1
Pages97-99
Secondary MarkB1_ASTRONOMIA_/_FÍSICA A2_GEOCIÊNCIAS B1_INTERDISCIPLINAR
History (UTC)2012-08-30 12:34:27 :: marciana -> administrator ::
2012-08-30 12:34:27 :: administrator -> marciana :: 2012
2013-01-18 14:32:51 :: marciana -> administrator :: 2012
2018-06-05 04:12:55 :: administrator -> marciana :: 2012
3. Content and structure
Is the master or a copy?is the master
Content Stagecompleted
Transferable1
Content TypeExternal Contribution
Version Typepublisher
KeywordsGeomagnetism
Magnetic fields
Solar system
Completely positive - Geometric storms - Interplanetary magnetic fields
Interplanetary parameters
Negative values
Positive value
AbstractThe interplanetary Bz(min) and geomagnetic Dst(min) are well related. There is no large negative Bz without causing large negative Dst. Similarly, large negative Dst is not expected to occur without a large negative Bz; but recently, Du et al. (2008) reported that the Dst storm of Jan. 21-22, 2005 was anomalous because the Dst storm main phase developed during northward interplanetary magnetic field (positive Bz). Here, we examined this event (storm 3) and compared it with earlier events of Jan. 16-20, 2005 (storms 1 and 2, in quick succession). It was noticed that storms 1 and 2 had large negative Dst deviations (-121 nT and -93 nT, separated by 26 hours) but the Bz fluctuated between 21 nT and -17 nT. For storm 3 where negative Dst deviations were large (-105 nT), the Bz was not completely positive (northward) as mentioned by Du et al. (2008) but had negative values (-7 nT) for an hour, followed by positive values (13 nT). Thus, the need of a negative Bz (albeit small) was satisfied.
AreaCEA
Arrangementurlib.net > BDMCI > Fonds > Produção anterior à 2021 > DIDGE > Interplanetary and geomagnetic...
doc Directory Contentaccess
source Directory Contentthere are no files
agreement Directory Content
agreement.html 30/08/2012 09:34 1.0 KiB 
4. Conditions of access and use
Languageen
User Groupadministrator
marciana
Reader Groupadministrator
marciana
Visibilityshown
Archiving Policydenypublisher denyfinaldraft24
Read Permissiondeny from all and allow from 150.163
Update Permissionnot transferred
5. Allied materials
Mirror Repositorysid.inpe.br/mtc-m19@80/2009/08.21.17.02.53
Next Higher Units8JMKD3MGPCW/3EU29DP
DisseminationWEBSCI; PORTALCAPES; COMPENDEX.
Host Collectionsid.inpe.br/mtc-m19@80/2009/08.21.17.02
6. Notes
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1. Identity statement
Reference TypeJournal Article
Sitemtc-m16d.sid.inpe.br
Holder Codeisadg {BR SPINPE} ibi 8JMKD3MGPCW/3DT298S
Identifier8JMKD3MGP7W/3CGDT2B
Repositorysid.inpe.br/mtc-m19/2012/08.24.14.48   (restricted access)
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Secondary KeyINPE--PRE/
DOI10.1016/j.pss.2012.05.011;
ISSN0032-0633
Citation KeyHessEcheZark:2012:SoWiPr
TitleSolar wind pressure effects on Jupiter decametric radio emissions independent of Io
ProjectFAPESP 2007/52533-1 e 2011/09403-3, CNPq 301233-2011-0)
Year2012
MonthSept.
Access Date2023, Jan. 31
Secondary TypePRE PI
Number of Files1
Size1545 KiB
2. Context
Author1 Hess, S. L. G.
2 Echer, E.
3 Zarka, P.
Group1
2 DGE-CEA-INPE-MCTI-GOV-BR
Affiliation1 LATMOS, IPSL-CNRS, Université Versailles-St Quentin, France
2 Instituto Nacional de Pesquisas Espaciais (INPE)
3 LESIA, Observatoire de Paris, CNRS, Univ. Paris-Diderot, Meudon, France
JournalPlanetary and Space Science
Volume70
Number1
Pages114-125
Secondary MarkB1_ASTRONOMIA_/_FÍSICA A2_GEOCIÊNCIAS B1_INTERDISCIPLINAR
History (UTC)2012-08-24 14:48:48 :: marciana -> administrator ::
2012-08-24 14:48:49 :: administrator -> marciana :: 2012
2012-12-05 11:56:44 :: marciana -> administrator :: 2012
2018-06-05 04:12:55 :: administrator -> marciana :: 2012
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KeywordsAuroral radio emissions
Electrodynamic interaction
Interplanetary fast shocks
Jovian magnetosphere
Jupiters
Michigan
Propagation models
Radio data
Radio emission
Solar wind dynamic pressure
Solar wind interactions
Solar wind pressure
Ultra-violet
Wind conditions
Decametric radio emission
Jupiter auroral radio emission
Jupiter magnetosphere
Solar wind
AbstractThis paper investigates the effects of the solar wind dynamic pressure on Jupiter auroral radio emissions at decametric wavelengths that are not controlled by the electrodynamic interaction with the moon Io (non-Io DAM). In order to conduct this study, Nanc¸ay decametric array radio data are analyzed for the 1996-1999 period. Solar wind conditions at Jupiter's orbit are studied using the Michigan University solar wind propagation model (mSWiM). Interplanetary fast shocks (forward shocks, FS, or reverse shocks, RS), and average solar wind dynamic pressure are correlated with non-Io DAM emission occurrence, duration and power. It is found that non-Io DAM emissions occur preferentially during periods of enhanced solar wind dynamic pressure and after a FS or a RS arrival at Jupiter. The dawn (non-Io B-type) and dusk (non-Io-A-type) radio emissions are investigated separately and show (1) a dawn-dusk asymmetry consistent with prior studies and auroral ultraviolet (UV) observations, and (2) different behaviors in response to solar wind shocks. Our study confirms the solar wind control of - at least a part of - the non-Io DAM, and refines the scenario of response of the radio emissions to the solar wind interaction with the Jovian magnetosphere.
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6. Notes
Empty Fieldsalternatejournal archivist callnumber copyholder copyright creatorhistory descriptionlevel e-mailaddress electronicmailaddress format isbn label lineage mark nextedition notes orcid parameterlist parentrepositories previousedition previouslowerunit progress resumeid rightsholder secondarydate session shorttitle sponsor subject targetfile tertiarymark tertiarytype typeofwork url
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1. Identity statement
Reference TypeJournal Article
Sitemtc-m16d.sid.inpe.br
Holder Codeisadg {BR SPINPE} ibi 8JMKD3MGPCW/3DT298S
Identifier8JMKD3MGP7W/3CGDA3H
Repositorysid.inpe.br/mtc-m19/2012/08.24.11.22   (restricted access)
Last Update2012:08.24.11.33.33 (UTC) marciana
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Secondary KeyINPE--PRE/
DOI10.1088/0031-8949/86/01/018405
ISSN0031-8949
Citation KeyRempelChiaBran:2012:LaChAB
TitleLagrangian chaos in an ABC-forced nonlinear dynamo
Year2012
MonthJuly
Access Date2023, Jan. 31
Secondary TypePRE PI
Number of Files1
Size2834 KiB
2. Context
Author1 Rempel, Erico L.
2 Chian, Abraham C-L
3 Brandenburg, Axel
Group1
2 DGE-CEA-INPE-MCTI-GOV-BR
Affiliation1 Institute of Aeronautical Technology (ITA), World Institute for Space Environment Research (WISER), 12228-900, São José dos Campos, SP, Brazil
2 Instituto Nacional de Pesquisas Espaciais (INPE)
3 NORDITA, AlbaNova University Ctr, Stockholm, Sweden
JournalPhysica Scripta
Volume86
Number1
PagesArticle number018405
History (UTC)2012-10-02 14:03:45 :: marciana -> administrator :: 2012
2012-10-19 20:28:37 :: administrator -> marciana :: 2012
2012-12-03 15:44:13 :: marciana -> administrator :: 2012
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KeywordsPlasma physics
Fluid dynamics
Interactive devices
Lagrange multipliers
Magnetohydrodynamics
Pollution control
Velocity. Statistical physics and nonlinear systems
AbstractThe Lagrangian properties of the velocity field in a magnetized fluid are studied using three-dimensional simulations of a helical magnetohydrodynamic dynamo. We compute the attracting and repelling Lagrangian coherent structures (LCS), which are dynamic lines and surfaces in the velocity field that delineate particle transport in flows with chaotic streamlines and act as transport barriers. Two dynamo regimes are explored, one with a robust coherent mean magnetic field and the other with intermittent bursts of magnetic energy. The LCS and the statistics of the finite-time Lyapunov exponents indicate that the stirring/mixing properties of the velocity field decay as a linear function of magnetic energy. The relevance of this study to the solar dynamo problem is also discussed.
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Next Higher Units8JMKD3MGPCW/3EU29DP
DisseminationWEBSCI; PORTALCAPES; COMPENDEX.
Host Collectionsid.inpe.br/mtc-m19@80/2009/08.21.17.02
6. Notes
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 resumeid rightsholder secondarydate secondarymark session shorttitle sponsor subject targetfile tertiarymark tertiarytype typeofwork url
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Reference TypeJournal Article
Sitemtc-m16d.sid.inpe.br
Holder Codeisadg {BR SPINPE} ibi 8JMKD3MGPCW/3DT298S
Identifier8JMKD3MGP7W/3CCCSH2
Repositorysid.inpe.br/mtc-m19/2012/07.30.18.45
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Secondary KeyINPE--PRE/
DOI10.1017/S174392131200484X
ISSN1743-9213
1743-9221
Citation KeyEcherTsurGonz:2012:ExLoGe
TitleExtremely low geomagnetic activity during the recent deep solar cycle minimum
ProjectCNPq (PQ-300211/2008-2) FAPESP (2008/06650-9)
Year2012
MonthJuly
Access Date2023, Jan. 31
Secondary TypePRE PI
Number of Files1
Size914 KiB
2. Context
Author1 Echer, Ezequiel
2 Tsurutani, Bruce T
3 Gonzalez, Walter D
Resume Identifier1 8JMKD3MGP5W/3C9JH3D
Group1 DGE-CEA-INPE-MCTI-GOV-BR
2
3 DGE-CEA-INPE-MCTI-GOV-BR
Affiliation1 Instituto Nacional de Pesquisas Espaciais (INPE)
2 Jet Propulsion Laboratory(JPL), California Institute of Technology (CALTECH) Pasadena, CA, USA
3 Instituto Nacional de Pesquisas Espaciais (INPE)
Author e-Mail Address1 ezequiel.echer@gmail.com
2 bruce.tsurutani@jpl.nasa.gov
3 gonzalez@dge.inpe.br
e-Mail Addresstereza@sid.inpe.br
JournalProceedings of the International Astronomical Union
Volume7
Number286
Pages200-209
History (UTC)2012-12-11 15:54:05 :: tereza@sid.inpe.br -> administrator :: 2012
2018-06-05 04:12:33 :: administrator -> tereza@sid.inpe.br :: 2012
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KeywordsSun: activity
Sun: magnetic fi




elds
solar-terrestrial relations
solar wind
AbstractAbstract. The recent solar minimum (2008-2009) was extreme in several aspects: the sunspot number, R z , interplanetary magnetic field (IMF) magnitude B o and solar wind speed V were the lowest during the space era. Furthermore, the variance of the IMF southward B component was low. As a consequence of these exceedingly low solar wind parameters, there was a minimum in the energy transfer from solar wind to the magnetosphere, and the geomagnetic activity ap index reached extremely low levels. The minimum in geomagnetic activity was delayed in relation to sunspot cycle minimum. We compare the solar wind and geomagnetic activity observed in this recent minimum with previous solar cycle values during the space era (1964-2010). Moreover, the geomagnetic activity conditions during the current minimum are compared with long term variability during the period of available geomagnetic observations. The extremely low geomagnetic activity observed in this solar minimum was previously recorded only at the end of XIX century and at the beginning of the XX century, and this might be related to the Gleissberg (80-100 years) solar cycle.
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data URLhttp://urlib.net/ibi/8JMKD3MGP7W/3CCCSH2
zipped data URLhttp://urlib.net/zip/8JMKD3MGP7W/3CCCSH2
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6. Notes
Empty Fieldsalternatejournal archivist callnumber copyholder copyright creatorhistory descriptionlevel format isbn label lineage mark nextedition notes orcid parameterlist parentrepositories previousedition previouslowerunit progress rightsholder secondarydate secondarymark session shorttitle sponsor subject targetfile tertiarymark tertiarytype typeofwork url
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Reference TypeJournal Article
Sitemtc-m16d.sid.inpe.br
Holder Codeisadg {BR SPINPE} ibi 8JMKD3MGPCW/3DT298S
Identifier8JMKD3MGP7W/3CCC4B2
Repositorysid.inpe.br/mtc-m19/2012/07.30.14.15
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Secondary KeyINPE--PRE/
DOI10.1103/PhysRevE.85.046406
ISSN1539-3755
Citation KeyAsenjoBoChMuVaRe:2012:SeNoWa
TitleSelf-modulation of nonlinear waves in a weakly magnetized relativistic electron-positron plasma with temperature
Year2012
MonthApr.
Access Date2023, Jan. 31
Secondary TypePRE PI
Number of Files1
Size2444 KiB
2. Context
Author1 Asenjo, Felipe A
2 Borotto, Felix A
3 Chian, Abraham C. -L.
4 Munoz, Victor
5 Valdivia, J. Alejandro
6 Rempel, Erico l
Group1
2
3 DGE-CEA-INPE-MCTI-GOV-BR
Affiliation1 Institute for Fusion Studies, University of Texas at Austin, Austin, Texas
2 Departamento de Física, Facultad de Ciencias Físicas y Matemáticas, Universidad de Concepción, Chile
3 Instituto Nacional de Pesquisas Espaciais (INPE)
4 Departamento de Física, Facultad de Ciencias, Universidad de Chile, Casilla 653, Santiago, Chile, and Centro para el Desarrollo de la Nanociencia y la Nanotecnología, CEDENNA
5 Departamento de Física, Facultad de Ciencias, Universidad de Chile, Casilla 653, Santiago, Chile, and Centro para el Desarrollo de la Nanociencia y la Nanotecnología, CEDENNA
6 Institute of Aeronautical Technology (ITA), 12228-900 São José dos Campos-SP
Author e-Mail Address1
2
3 achian@dge.inpe.br
e-Mail Addresstereza@sid.inpe.br
JournalPhysical Review E
Volume85
Number4
Pages046406/1-046406/6
Secondary MarkB1_ASTRONOMIA_/_FÍSICA B2_CIÊNCIA_DA_COMPUTAÇÃO B1_CIÊNCIAS_BIOLÓGICAS_I B1_CIÊNCIAS_BIOLÓGICAS_II B1_ECONOMIA A2_ENGENHARIAS_II A1_ENGENHARIAS_III B1_ENGENHARIAS_IV A2_FARMÁCIA A2_GEOCIÊNCIAS A1_INTERDISCIPLINAR A2_MATEMÁTICA_/_PROBABILIDADE_E_ESTATÍSTICA A2_MATERIAIS A2_MEDICINA_I A2_MEDICINA_II B1_QUÍMICA
History (UTC)2012-07-30 14:15:09 :: tereza@sid.inpe.br -> administrator ::
2012-07-30 14:15:09 :: administrator -> tereza@sid.inpe.br :: 2012
2012-07-30 14:23:16 :: tereza@sid.inpe.br -> administrator :: 2012
2012-07-30 15:42:17 :: administrator -> tereza@sid.inpe.br :: 2012
2012-08-24 11:45:39 :: tereza@sid.inpe.br -> banon :: 2012
2012-09-27 17:56:49 :: banon -> administrator :: 2012
2012-10-19 20:28:18 :: administrator -> tereza@sid.inpe.br :: 2012
2013-01-20 15:25:27 :: tereza@sid.inpe.br -> banon :: 2012
2013-01-20 15:26:26 :: banon -> administrator :: 2012
2018-06-05 04:12:33 :: administrator -> tereza@sid.inpe.br :: 2012
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Keywordselectromagnetic waves
magnetized electron-positron plasma
high-energy astrophysics
AbstractWe develop a nonlinear theory for self-modulation of a circularly polarized electromagnetic wave in a relativistic hot weakly magnetized electron-positron plasma. The case of parallel propagation along an ambient magnetic field is considered. A nonlinear Schrödinger equation is derived for the complex wave amplitude of a self-modulated wave packet. We show that the maximum growth rate of the modulational instability decreases as the temperature of the pair plasma increases. Depending on the initial conditions, the unstable wave envelope can evolve nonlinearly to either periodic wave trains or solitary waves. This theory has application to high-energy astrophysics and high-power laser physics.
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Arrangementurlib.net > BDMCI > Fonds > Produção anterior à 2021 > DIDGE > Self-modulation of nonlinear...
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URL (untrusted data)http://link.aps.org/doi/10.1103/PhysRevE.85.046406
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