Resultado da Pesquisa
A expressão de busca foi <secondaryty pi and firstg DGE-CEA-INPE-MCTI-GOV-BR and y 2013 and dissemination websci>.
25 referências foram encontradas buscando em 15 dentre 15 sites
(este total pode incluir algumas duplicatas - para ver a conta certa clique no botão Mostrar Todas).
As 10 mais recentes estão listadas abaixo.
Data e hora local de busca: 24/02/2021 21:01.

Área de identificação
Tipo de ReferênciaJournal Article
Sitemtc-m21b.sid.inpe.br
Código do Detentorisadg {BR SPINPE} ibi 8JMKD3MGPCW/3DT298S
Identificador8JMKD3MGP5W34M/3FA462E
Repositóriosid.inpe.br/mtc-m21b/2013/11.26.17.01.42
Última Atualização2015:03.12.17.23.58 marcelo.pazos@inpe.br
Metadadossid.inpe.br/mtc-m21b/2013/11.26.17.01.43
Última Atualização dos Metadados2020:09.09.10.49.03 marcelo.pazos@inpe.br
DOI10.1002/grl.50904
ISSN0094-8276
Rótuloscopus 2013-11
Chave de CitaçãoCamposSaba:2013:ViChDe
TítuloVisible channel development during the initial breakdown of a natural negative cloud-to-ground flash
Ano2013
Data de Acesso24 fev. 2021
Tipo de Trabalhojournal article
Número de Arquivos1
Tamanho1162 KiB
Área de contextualização
Autor1 Campos, Leandro Zanella de Souza
2 Saba, Marcelo Magalhães Fares
Identificador de Curriculo1
2 8JMKD3MGP5W/3C9JHP6
Grupo1 DGE-CEA-INPE-MCTI-GOV-BR
2 CST-CST-INPE-MCTI-GOV-BR
Afiliação1 Instituto Nacional de Pesquisas Espaciais (INPE)
2 Instituto Nacional de Pesquisas Espaciais (INPE)
Endereço de e-Mail do Autor1 leandro.zanella@gmail.com
2 marcelo.saba@inpe.br
Endereço de e-Mailmarcelo.pazos@inpe.br
RevistaGeophysical Research Letters
Volume40
Número17
Páginas4756-4761
Tipo SecundárioPRE PI
Nota SecundáriaA1 A1 A1 A1 A1 A1 A1 A2 A2 A2 A2 A2 B1
Histórico2018-06-04 03:14:13 :: administrator -> marcelo.pazos@inpe.br :: 2013
2020-09-09 10:49:03 :: marcelo.pazos@inpe.br -> simone :: 2013
Área de conteúdo e estrutura
É a matriz ou uma cópia?é a matriz
Estágio do Conteúdoconcluido
Transferível1
Tipo do ConteudoExternal Contribution
Tipo de Versãopublisher
Palavras-ChaveCloud-to-ground flash, Electric field waveform, Frames per seconds, initial breakdown, Initial breakdown pulse, Initial development, leader, Leader development, Electric fields, Lightning, cloud, cloud to ground lightning, electric field, GPS, lightning, thundercloud.
ResumoGPS time synchronized high-speed video records (at 4000 frames per second) and electric field waveforms are discussed for one stepped leader of a negative cloud-to-ground flash whose initial development becomes visible above cloud base. The leader emerges from the opaque region of the thundercloud around 4800 m above ground, propagating with speeds of the order of 106 m s -1. It is possible to see that this early, bright, and fast propagation period occurred simultaneously with the emission of initial breakdown bipolar pulse trains. The leader gradually reduces its speed and luminous intensity: When its tip is less than 3000 m above the ground, the propagation speeds oscillate between 2 and 4 × 105 m s -1 until it makes contact approximately 16 ms after it first became visible. With time, the initial breakdown waveform is gradually replaced by unipolar pulses and the leader propagation speed drops to the 105 m s-1 range. Key Points Fast visible leader development during the initial breakdown pulse activity Breakdown bipolar pulse trains become unipolar as the leader slows down.
AreaCEA
Arranjo 1INPE > Produção > DIDGE > Visible channel development...
Arranjo 2INPE > Produção > COCST > Visible channel development...
Conteúdo da Pasta sourcenão têm arquivos
Conteúdo da Pasta agreementnão têm arquivos
Área de condições de acesso e uso
URL dos dadoshttp://urlib.net/rep/8JMKD3MGP5W34M/3FA462E
URL dos dados zipadoshttp://urlib.net/zip/8JMKD3MGP5W34M/3FA462E
Idiomaen
Arquivo Alvocampos_visible.pdf
Grupo de Usuáriosadministrator
marcelo.pazos@inpe.br
simone
Visibilidadeshown
Política de Arquivamentodenypublisher6 allowfinaldraft
Permissão de Leituraallow from all
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Área de fontes relacionadas
Repositório Espelhoiconet.com.br/banon/2006/11.26.21.31
Unidades Imediatamente Superiores8JMKD3MGPCW/3EU29DP
8JMKD3MGPCW/3F3T29H
DivulgaçãoWEBSCI; AGU; MGA; COMPENDEX; SCOPUS.
Acervo Hospedeirosid.inpe.br/mtc-m21b/2013/09.26.14.25.20
Área de notas
Campos Vaziosalternatejournal archivist callnumber copyholder copyright creatorhistory descriptionlevel format isbn lineage mark month nextedition notes orcid parameterlist parentrepositories previousedition previouslowerunit progress project readergroup rightsholder secondarydate secondarykey session shorttitle sponsor subject tertiarymark tertiarytype url
Área de identificação
Tipo de ReferênciaJournal Article
Sitemtc-m16d.sid.inpe.br
Código do Detentorisadg {BR SPINPE} ibi 8JMKD3MGPCW/3DT298S
Identificador8JMKD3MGP7W/3ECH7E5
Repositóriosid.inpe.br/mtc-m19/2013/06.28.21.50   (acesso restrito)
Última Atualização2013:06.28.21.50.29 administrator
Metadadossid.inpe.br/mtc-m19/2013/06.28.21.50.29
Última Atualização dos Metadados2018:06.05.04.14.24 administrator
DOI10.1016/j.asr.2012.11.023
ISSN0273-1177
Rótuloself-archiving-INPE-MCTI-GOV-BR
Chave de CitaçãoDalLagoGoLuBrViStRo:2013:CMDyUs
TítuloCME dynamics using coronagraph and interplanetary ejecta data
ProjetoCNPq (305351/2011-7; 481368/2010-8); FAPESP (2009/14995-9; 2009/12869-6; 2010/13707-7)
Ano2013
MêsMay
Data de Acesso24 fev. 2021
Número de Arquivos1
Tamanho403 KiB
Área de contextualização
Autor1 Dal Lago, Alisson
2 Gonzalez, Walter Demétrio
3 Lucas, Aline De
4 Braga, Carlos Roberto
5 Vieira, Lucas Ramos
6 Stekel, Tardelli Ronan Coelho
7 Rockenbach, Marlos
Identificador de Curriculo1 8JMKD3MGP5W/3C9JGH3
2 8JMKD3MGP5W/3C9JJC4
Grupo1 DGE-CEA-INPE-MCTI-GOV-BR
2 DGE-CEA-INPE-MCTI-GOV-BR
3 DGE-CEA-INPE-MCTI-GOV-BR
4 GESAST-CEA-SPG-INPE-MCTI-GOV-BR
5 GESAST-CEA-SPG-INPE-MCTI-GOV-BR
6 GESAST-CEA-SPG-INPE-MCTI-GOV-BR
Afiliação1 Instituto Nacional de Pesquisas Espaciais (INPE)
2 Instituto Nacional de Pesquisas Espaciais (INPE)
3 Instituto Nacional de Pesquisas Espaciais (INPE)
4 Instituto Nacional de Pesquisas Espaciais (INPE)
5 Instituto Nacional de Pesquisas Espaciais (INPE)
6 Instituto Nacional de Pesquisas Espaciais (INPE)
7 Instituto de Pesquisa e Desenvolvimento, Universidade do Vale do Paraı´ba, Sa˜o Jose´ dos Campos, Brazil
Endereço de e-Mail do Autor1 dallago@dge.inpe.br
2 gonzalez@dge.inpe.br
3 delucas@dge.inpe.br
4 crbraga@dge.inpe.br
5 lucasfisico@gmail.com
6 tardellirs@gmail.com
7 marlosrs@gmail.com
Endereço de e-Mailoswaldo@das.inpe.br
RevistaAdvances in Space Research
Volume51
Número10
Páginas1942–1948
Tipo SecundárioPRE PI
Nota SecundáriaB1 B1 B1 B1 B2 B3 B4
Histórico2013-06-28 21:50:29 :: oswaldo@das.inpe.br -> administrator ::
2018-06-05 04:14:24 :: administrator -> marcelo.pazos@inpe.br :: 2013
Área de conteúdo e estrutura
É a matriz ou uma cópia?é a matriz
Estágio do Conteúdoconcluido
Transferível1
Tipo do ConteudoExternal Contribution
Tipo de Versãopublisher
Palavras-Chavecoronal mass ejection, interplanetary ejecta, CME travel time models, space weather.
ResumoIn this work, we present a study of the coronal mass ejection (CME) dynamics using LASCO coronagraph observations combined with in-situ ACE plasma and magnetic field data, covering a continuous period of time from January 1997 to April 2001, complemented by few extreme events observed in 2001 and 2003. We show, for the first time, that the CME expansion speed correlates very well with the travel time to 1 AU of the interplanetary ejecta (or ICMEs) associated with the CMEs, as well as with their preceding shocks. The events analyzed in this work are a subset of the events studied in Schwenn et al. (2005), from which only the CMEs associated with interplanetary ejecta (ICMEs) were selected. Three models to predict CME travel time to Earth, two proposed by Gopalswamy et al. (2001) and one by Schwenn et al. (2005), were used to characterize the dynamical behavior of this set of events. Extreme events occurred in 2001 and 2003 were used to test the prediction capability of the models regarding CMEs with very high LASCO C3 speeds.
AreaCEA
Conteúdo da Pasta sourcenão têm arquivos
Conteúdo da Pasta agreement
agreement.html 28/06/2013 18:50 1.0 KiB 
Área de condições de acesso e uso
Idiomaen
Arquivo Alvo1-s2.0-S0273117712007065-main.pdf
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marcelo.pazos@inpe.br
oswaldo@das.inpe.br
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Visibilidadeshown
Política de Arquivamentodenypublisher denyfinaldraft24
Permissão de Leituradeny from all and allow from 150.163
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Repositório Espelhoiconet.com.br/banon/2006/11.26.21.31
Unidades Imediatamente Superiores8JMKD3MGPCW/3EU29DP
8JMKD3MGPCW/3F2PBEE
8JMKD3MGPCW/3F2PF8L
8JMKD3MGPCW/3F2PG65
URL (dados não confiáveis)http://dx.doi.org/10.1016/j.asr.2012.11.023
DivulgaçãoWEBSCI; PORTALCAPES; MGA; COMPENDEX; SCOPUS.
Acervo Hospedeirosid.inpe.br/mtc-m19@80/2009/08.21.17.02
Área de notas
Campos Vaziosalternatejournal archivist callnumber copyholder copyright creatorhistory descriptionlevel format isbn lineage mark nextedition notes orcid parameterlist parentrepositories previousedition previouslowerunit progress rightsholder secondarydate secondarykey session shorttitle sponsor subject tertiarymark tertiarytype typeofwork
Área de controle da descrição
e-Mail (login)marcelo.pazos@inpe.br
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Área de identificação
Tipo de ReferênciaJournal Article
Sitemtc-m16d.sid.inpe.br
Código do Detentorisadg {BR SPINPE} ibi 8JMKD3MGPCW/3DT298S
Identificador8JMKD3MGP7W/3E9Q9L3
Repositóriosid.inpe.br/mtc-m19/2013/06.12.01.41.16
Última Atualização2014:03.27.13.50.09 administrator
Metadadossid.inpe.br/mtc-m19/2013/06.12.01.41.17
Última Atualização dos Metadados2018:06.05.04.14.18 administrator
DOI10.1029/2012JA018086
ISSN0148-0227
2156-2202
Rótuloisi
Chave de CitaçãoEcherTsurGonz:2013:InOrMo
TítuloInterplanetary origins of moderate (-100 nT < Dst <=-50 nT) geomagnetic storms during solar cycle 23 (1996-2008)
ProjetoCNPq (301233/2011-0)
Ano2013
MêsJan.
Data de Acesso24 fev. 2021
Tipo de Trabalhojournal article
Número de Arquivos1
Tamanho2020 KiB
Área de contextualização
Autor1 Echer, Ezequiel
2 Tsurutani, Bruce T.
3 Gonzalez, Walter Demétrio
Identificador de Curriculo1 8JMKD3MGP5W/3C9JH3D
2
3 8JMKD3MGP5W/3C9JJC4
Grupo1
2
3 DGE-CEA-INPE-MCTI-GOV-BR
Afiliação1 Instituto Nacional de Pesquisas Espaciais (INPE)
2 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
3 Natl Inst Space Res INPE, BR-12227010 Sao Jose Dos Campos, SP, Brazil.
Endereço de e-Mail do Autor1 eecher@dge.inpe.br
2 bruce.tsurutani@jpl.nasa.gov
3 gonzalez@dge.inpe.br
Endereço de e-Mailmarcelo.pazos@inpe.br
RevistaJournal of Geophysical Research
Volume118
Número1
Páginas385-392
Tipo SecundárioPRE PI
Histórico2018-06-05 04:14:18 :: administrator -> marcelo.pazos@inpe.br :: 2013
Área de conteúdo e estrutura
É a matriz ou uma cópia?é a matriz
Estágio do Conteúdoconcluido
Transferível1
Tipo do ConteudoExternal Contribution
Tipo de Versãofinaldraft
Palavras-Chavegeomagnetic storms, solar wind, magnetosphere, solar cycle, space weather.
ResumoThe interplanetary causes of 213 moderate-intensity (-100 nT < peak Dst <= -50 nT) geomagnetic storms that occurred in solar cycle 23 (1996-2008) are identified. Interplanetary drivers such as corotating interaction regions (CIRs), pure high-speed streams (HSSs), interplanetary coronal mass ejections (ICMEs) of two types [those with magnetic clouds (MCs) and those without (nonmagnetic cloud or ICME\_nc)], sheaths (compressed and/or draped sheath fields), as well as their combined occurrence were identified as causes of the storms. The annual rate of occurrence of moderate storms had two peaks, one near solar maximum and the other in the descending phase, around 3 years later. The highest rate of moderate storm occurrence was found in the declining phase (25 storms year(-1)). The lowest occurrence rate was 5.7 storms year(-1) and occurred at solar minimum. All moderate-intensity storms were associated with southward interplanetary magnetic fields, indicating that magnetic reconnection was the main mechanism for solar wind energy transfer to the magnetosphere. Most of these storms were associated with CIRs and pure HSSs (47.9\%), followed by MCs and noncloud ICMEs (20.6\%), pure sheath fields (10.8\%), and sheath and ICME combined occurrence (9.9\%). In terms of solar cycle dependence, CIRs and HSSs are the dominant drivers in the declining phase and at solar minimum. CIRs and HSSs combined have about the same level of importance as ICMEs plus their sheaths in the rising and maximum solar cycle phases. Thus, CIRs and HSSs are the main driver of moderate storms throughout a solar cycle but with variable contributions from ICMEs, their shocks (sheaths), and combined occurrence within the solar cycle. This result is significantly different than that for intense (Dst <= -100 nT) and superintense (Dst <= -250 nT) magnetic storms shown in previous studies. For superintense geomagnetic storms, 100\% of the events were due to ICME events, while for intense storms, ICMEs, sheaths, and their combination caused almost 80\% of the storms. CIRs caused only 13\% of the intense storms. The typical interplanetary electric field (Ey) criteria for moderate magnetic storms were identified. It was found that similar to 80.1\% of the storms follow the criterion of Ey >= 2 mV m(-1) for intervals longer than 2 h. It is concluded that southward directed interplanetary magnetic fields within CIRs/HSSs may be the main energy source for long-term averaged geomagnetic activity on Earth. Citation: Echer E., B. T. Tsurutani and W. D. Gonzalez (2013), Interplanetary origins of moderate (-100 nT < Dst -50 nT) geomagnetic storms during solar cycle 23 (1996-2008), J. Geophys. Res. Space Physics, 118, 385-392, doi:10.1029/2012JA018086.
AreaCEA
Conteúdo da Pasta sourcenão têm arquivos
Conteúdo da Pasta agreementnão têm arquivos
Área de condições de acesso e uso
URL dos dadoshttp://urlib.net/rep/8JMKD3MGP7W/3E9Q9L3
URL dos dados zipadoshttp://urlib.net/zip/8JMKD3MGP7W/3E9Q9L3
Idiomaen
Arquivo Alvo727835_2_merged_1352834001.pdf
Grupo de Usuáriosadministrator
marcelo.pazos@inpe.br
self-uploading-INPE-MCTI-GOV-BR
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marcelo.pazos@inpe.br
Visibilidadeshown
Política de Arquivamentodenypublisher6 allowfinaldraft
Permissão de Leituraallow from all
Permissão de Atualizaçãonão transferida
Área de fontes relacionadas
Repositório Espelhoiconet.com.br/banon/2006/11.26.21.31
Unidades Imediatamente Superiores8JMKD3MGPCW/3EU29DP
DivulgaçãoWEBSCI; AGU; MGA; COMPENDEX; SCOPUS.
Acervo Hospedeirosid.inpe.br/mtc-m19@80/2009/08.21.17.02
Área de notas
Campos Vaziosalternatejournal archivist callnumber copyholder copyright creatorhistory descriptionlevel format isbn lineage mark nextedition notes orcid parameterlist parentrepositories previousedition previouslowerunit progress rightsholder secondarydate secondarykey secondarymark session shorttitle sponsor subject tertiarymark tertiarytype url
Área de controle da descrição
e-Mail (login)marcelo.pazos@inpe.br
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Área de identificação
Tipo de ReferênciaJournal Article
Sitemtc-m16d.sid.inpe.br
Código do Detentorisadg {BR SPINPE} ibi 8JMKD3MGPCW/3DT298S
Identificador8JMKD3MGP7W/3E9B982
Repositóriosid.inpe.br/mtc-m19/2013/06.09.02.31.12
Última Atualização2013:07.16.16.59.42 administrator
Metadadossid.inpe.br/mtc-m19/2013/06.09.02.31.13
Última Atualização dos Metadados2018:06.05.04.14.14 administrator
DOI10.1103/PhysRevE.87.022821
ISSN1539-3755
Rótuloscopus
Chave de CitaçãoToledoChReMiMuVa:2013:EaTs27
TítuloWavelet-based multifractal analysis of nonlinear time series: The earthquake-driven tsunami of 27 February 2010 in Chile
ProjetoFAPESP (2010/09405-5); CNPq (301634/2011-4); FAPESP (2011/50714-4); FAPESP (2011/10466-1); FAPESP (2010/00214-2).
Ano2013
Data de Acesso24 fev. 2021
Número de Arquivos1
Tamanho1786 KiB
Área de contextualização
Autor1 Toledo, B. A.
2 Chian, Abraham Chian-Long
3 Rempel, E. L.
4 Miranda, R. A.
5 Muñoz, P. R.
6 Valdivia, J. A.
Grupo1
2 DGE-CEA-INPE-MCTI-GOV-BR
Afiliação1 Institute of Aeronautical Technology (ITA), World Institute for Space Environment Research (WISER), CTA/ITA/IEFM, São José dos Campos-SP 12228-900, Brazil; Departamento de Física, Facultad de Ciencias, Universidad de Chile, Las Palmeras 3425, Ñuñoa, Santiago, Chile
2 Instituto Nacional de Pesquisas Espaciais (INPE)
3 Institute of Aeronautical Technology (ITA), World Institute for Space Environment Research (WISER), CTA/ITA/IEFM, São José dos Campos-SP 12228-900, Brazil
4 Institute of Aeronautical Technology (ITA), World Institute for Space Environment Research (WISER), CTA/ITA/IEFM, São José dos Campos-SP 12228-900, Brazil; Plasma Physics Laboratory, Institute of Physics, University of Brasília (UnB), Brasília-DF 70910-900, Brazil
5 Institute of Aeronautical Technology (ITA), World Institute for Space Environment Research (WISER), CTA/ITA/IEFM, São José dos Campos-SP 12228-900, Brazil
6 Departamento de Física, Facultad de Ciencias, Universidad de Chile, Las Palmeras 3425, Ñuñoa, Santiago, Chile
Endereço de e-Mail do Autor1 btoledo@fisica.ciencias.uchile.cl
2 achian@dge.inpe.br
Endereço de e-Mailmarcelo.pazos@inpe.br
RevistaPhysical Review E
Volume87
Número2
Páginas022821
Tipo SecundárioPRE PI
Nota SecundáriaA1 A2 A2 A2 A2 A2 A2 B1 B1 B1 B1 B1 B1 B1 B1 B1 B1 B1 C
Histórico2018-06-05 04:14:14 :: administrator -> marcelo.pazos@inpe.br :: 2013
Área de conteúdo e estrutura
É a matriz ou uma cópia?é a matriz
Estágio do Conteúdoconcluido
Transferível1
Tipo do ConteudoExternal Contribution
Tipo de Versãopublisher
Palavras-ChaveBiomedical signal, Discrete wavelets, Dynamical similarity, Dynamical state, Multi-fractal property, Multifractal analysis, Nonlinear time series, Numerical solution, Off state, On state, On-off intermittency, Regularized long wave equation, Shallow-water dynamics, Sudden change, Two-state, Wavelet leader, Bioelectric phenomena, Fractals, Gages, Nonlinear dynamical systems, Sea level, Time series, Waves, Tsunamis.
ResumoWe study general multifractal properties of tidal gauge and long-wave time series which show a well defined transition between two states, as is the case of sea level when a tsunami arrives. We adopt a method based on discrete wavelets, called wavelet leaders, which has been successfully used in a wide range of applications from image analysis to biomedical signals. First, we analyze an empirical time series of tidal gauge from the tsunami event of 27 February 2010 in Chile. Then, we study a numerical solution of the driven-damped regularized long-wave equation (RLWE) which displays on-off intermittency. Both time series are characterized by a sudden change between two sharply distinct dynamical states. Our analysis suggests a correspondence between the pre- and post-tsunami states (ocean background) and the on state in the RLWE, and also between the tsunami state (disturbed ocean) and the off state in the RLWE. A qualitative similarity in their singularity spectra is observed, and since the RLWE is used to model shallow water dynamics, this result could imply an underlying dynamical similarity.
AreaCEA
Conteúdo da Pasta sourcenão têm arquivos
Conteúdo da Pasta agreementnão têm arquivos
Área de condições de acesso e uso
URL dos dadoshttp://urlib.net/rep/8JMKD3MGP7W/3E9B982
URL dos dados zipadoshttp://urlib.net/zip/8JMKD3MGP7W/3E9B982
Idiomaen
Arquivo AlvoPhysRevE.87.022821.pdf
Grupo de Usuáriosadministrator
marcelo.pazos@inpe.br
Grupo de Leitoresadministrator
marcelo.pazos@inpe.br
Visibilidadeshown
Política de Arquivamentoallowpublisher allowfinaldraft
Permissão de Leituraallow from all
Permissão de Atualizaçãonão transferida
Área de fontes relacionadas
Repositório Espelhoiconet.com.br/banon/2006/11.26.21.31
Unidades Imediatamente Superiores8JMKD3MGPCW/3EU29DP
DivulgaçãoWEBSCI; PORTALCAPES; COMPENDEX; SCOPUS.
Acervo Hospedeirosid.inpe.br/mtc-m19@80/2009/08.21.17.02
Área de notas
Campos Vaziosalternatejournal archivist callnumber copyholder copyright creatorhistory descriptionlevel format isbn lineage mark month nextedition notes orcid parameterlist parentrepositories previousedition previouslowerunit progress resumeid rightsholder secondarydate secondarykey session shorttitle sponsor subject tertiarymark tertiarytype typeofwork url
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e-Mail (login)marcelo.pazos@inpe.br
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Área de identificação
Tipo de ReferênciaJournal Article
Sitemtc-m16d.sid.inpe.br
Código do Detentorisadg {BR SPINPE} ibi 8JMKD3MGPCW/3DT298S
Identificador8JMKD3MGP7W/3E9B7NN
Repositóriosid.inpe.br/mtc-m19/2013/06.09.02.13.32   (acesso restrito)
Última Atualização2013:06.10.18.01.31 administrator
Metadadossid.inpe.br/mtc-m19/2013/06.09.02.13.33
Última Atualização dos Metadados2018:06.05.04.14.11 administrator
DOI10.1016/j.asr.2012.03.007
ISSN0273-1177
Rótuloscopus
Chave de CitaçãoMirandaChiaRemp:2013:UnScLa
TítuloUniversal scaling laws for fully-developed magnetic field turbulence near and far upstream of the Earth's bow shock
Ano2013
Data de Acesso24 fev. 2021
Número de Arquivos1
Tamanho697 KiB
Área de contextualização
Autor1 Miranda, R. A.
2 Chian, Abraham Chian Long
3 Rempel, E. L.
Grupo1
2 DGE-CEA-INPE-MCTI-GOV-BR
Afiliação1 Institute of Aeronautical Technology (ITA), World Institute for Space Environment Research (WISER), São José dos Campos-SP 12228-900, Brazil; University of Brasília (UnB), Faculty of Technology, Campus Gama, Brasília-DF 70910-900, Brazil
2 Instituto Nacional de Pesquisas Espaciais (INPE)
3 Institute of Aeronautical Technology (ITA), World Institute for Space Environment Research (WISER), São José dos Campos-SP 12228-900, Brazil; National Institute for Space Research (INPE), World Institute for Space Environment Research (WISER), São José dos Campos-SP 12227-010, Brazil
Endereço de e-Mailmarcelo.pazos@inpe.br
RevistaAdvances in Space Research
Volume51
Número10
Páginas1893-1901
Tipo SecundárioPRE PI
Nota SecundáriaB1 B1 B1 B1 B2 B3 B4
Histórico2018-06-05 04:14:11 :: administrator -> marcelo.pazos@inpe.br :: 2013
Área de conteúdo e estrutura
É a matriz ou uma cópia?é a matriz
Estágio do Conteúdoconcluido
Transferível1
Tipo do ConteudoExternal Contribution
Tipo de Versãopublisher
Palavras-ChaveDissipative structure, High order statistics, Intermittency, Interplanetary magnetic fields, Magnetohydrodynamic turbulence, Multi fractals, Solar wind plasmas, Universal scaling laws, Fractals, Magnetic fields, Magnetohydrodynamics, Magnetoplasma, Plasma shock waves, Scaling laws, Solar wind, Turbulence.
ResumoWe analyze the multifractal scaling of the modulus of the interplanetary magnetic field near and far upstream of the Earth's bow shock, measured by Cluster and ACE, respectively, from 1 to 3 February 2002. The maximum order of the structure function is carefully estimated for each time series using two different techniques, to ensure the validity of our high-order statistics. The first technique consists of plotting the integrand of the pth order structure function, and the second technique is a quantitative method which relies on the power-law scaling of the extreme events. We compare the scaling exponents computed from the structure functions of magnetic field differences with the predictions obtained by the She-Lévêque model of intermittency in anisotropic magnetohydrodynamic turbulence. Our results show a good agreement between the model and the observations near and far upstream of the Earth's bow shock, rendering support for the modelling of universal scaling laws based on the Kolmogorov phenomenology in the presence of sheet-like dissipative structures.
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DOI10.1016/j.asr.2012.05.009
ISSN0273-1177
Rótuloscopus
Chave de CitaçãoBragaDalLSten:2013:PsChMo
TítuloPseudo-automatic characterization of the morphological and kinematical properties of coronal mass ejections using a texture-based technique
Ano2013
Data de Acesso24 fev. 2021
Número de Arquivos1
Tamanho1060 KiB
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Autor1 Braga, C. R.
2 Dal Lago, Alisson
3 Stenborg, G.
Identificador de Curriculo1
2 8JMKD3MGP5W/3C9JGH3
Grupo1
2 DGE-CEA-INPE-MCTI-GOV-BR
Afiliação1 National Institute for Space Research-INPE, Av. dos Astronautas, 1758, Sao Jose dos Campos, SP, Brazil
2 National Institute for Space Research-INPE, Av. dos Astronautas, 1758, Sao Jose dos Campos, SP, Brazil
3 School of Physics, Astronomy and Computational Sciences, George Mason University, Fairfax, VA 22030, United States
Endereço de e-Mailmarcelo.pazos@inpe.br
RevistaAdvances in Space Research
Volume51
Número10
Páginas1949-1965
Tipo SecundárioPRE PI
Nota SecundáriaB1 B1 B1 B1 B2 B3 B4
Histórico2018-06-05 04:14:11 :: administrator -> marcelo.pazos@inpe.br :: 2013
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Palavras-ChaveAutomatic computations, Coronal mass ejection, CORSET, Detection and tracking, Kinematic characterization, Kinematic properties, Segmentation techniques, Supervised segmentation, Automation, Characterization, Kinematics, Textures, Parameter estimation.
ResumoThe white light coronagraphs onboard SOHO (LASCO-C2 and -C3) and most recently STEREO (SECCHI -COR1 and -COR2) have detected a myriad of coronal mass ejections (CME). They are a key component of space weather and under certain conditions they can become geo-effective, hence the importance of their kinematic characterization to help predict their effects. However, there is still a lot of debate on how to define the event boundaries for space weather purposes, which in turn makes it difficult to agree on their kinematic properties. That lack of agreement is reflected in both the manual and automated CME catalogs in existence. To contribute to a more objective definition and characterization of white-light coronagraph events, Goussies et al. (2010) introduced recently the concept of "texture of the event". Based on that property, they developed a supervised segmentation algorithm to allow the automatic tracking of dynamic events observed in the coronagraphs field of view, which is called CORonal SEgmentation Technique (CORSET). In this work, we have enhanced the capabilities of the algorithm by adding several new functionalities, namely the automatic computation of different morphological and kinematic parameters. We tested its performance on 57 well-studied limb CME events observed with the LASCO coronagraphs between 1997 and 2001, and compared the parameters obtained with those from three existent CME lists: two of them obtained from an observer-based detection and tracking method (i.e.; two manual catalogs), and the other one based on the automated detection and characterization of the CME events (i.e.; a fully automated catalog). We found that 51 events could be tracked and quantified in agreement with the CME definition. In general terms, the position angle, and the radial and expansion speeds are in agreement with the manual catalogs used for comparison. On the other hand, some discrepancies between CORSET and the automated catalog were found, which can be explained by the different delimitation of the CME angular extent.
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Repositóriosid.inpe.br/mtc-m19/2013/06.09.02.13.28   (acesso restrito)
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DOI10.1016/j.asr.2012.10.029
ISSN0273-1177
Rótuloscopus
Chave de CitaçãoGonzalezGonz:2013:LoVaGe
TítuloLocal-time variations of geomagnetic disturbances during intense geomagnetic storms and possible association with their interplanetary causes
ProjetoFundo de Desenvolvimento Científico e Tecnológico e Conselho Nacional de Desenvolvimento Científico e Tecnológico (PQ-342734/2008-2 e PQ-300321/2005-8)
Ano2013
Data de Acesso24 fev. 2021
Tipo de Trabalhojournal article
Número de Arquivos1
Tamanho3869 KiB
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Autor1 Gonzalez, Alicia Luisa Clua de
2 Gonzalez, Walter Demetrio
Identificador de Curriculo1
2 8JMKD3MGP5W/3C9JJC4
Grupo1 DGE-CEA-INPE-MCTI-GOV-BR
2 DGE-CEA-INPE-MCTI-GOV-BR
Afiliação1 Instituto Nacional de Pesquisas Espaciais (INPE)
2 Instituto Nacional de Pesquisas Espaciais (INPE)
Endereço de e-Mail do Autor1 alicia@dge.inpe.br
2 gonzalez@dge.inpe.br
Endereço de e-Mailmarcelo.pazos@inpe.br
RevistaAdvances in Space Research
Volume51
Número10
Páginas1924-1933
Tipo SecundárioPRE PI
Nota SecundáriaB1 B1 B1 B1 B2 B3 B4
Histórico2018-06-05 04:14:11 :: administrator -> marcelo.pazos@inpe.br :: 2013
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Palavras-Chavegeomagnetic disturbance, geomagnetic fields, geomagnetic indices, intense geomagnetic storms, mid-latitude station, relative intensity, solar-terrestrial relations, temporal evolution, solar energy, storms, geomagnetism.
ResumoIn the present paper the local-time variations in the disturbance of the geomagnetic-field horizontal component (H) for eight intense geomagnetic storms that occurred during the descending phase of solar cycle 23 have been analyzed. The study was based on the plot of contour lines of the H-depletion intensity in the plane local time versus universal time (LT-UT maps) with the objective of observing how the morphology and evolution of the ring current is mapped into the surface of the Earth in presence of intense geomagnetic storms. The criterion for the selection of the events was a peak Dst below about-200 nT. The values of the horizontal geomagnetic field were obtained from six mid-latitude stations, with 1 min resolution, and the disturbances were computed by a process similar to that for obtaining the Sym-H geomagnetic index. By means of a cubic spline, the results were interpolated to all longitudes with 6 min in LT spacement. The observed contour maps show, as expected, that the region of largest depletion in H are situated around dusk, as a consequence of the formation of a partial ring current, mainly located in the noon-dusk-midnight hemisphere. However, H disturbances are also observed around midnight and, to a less extend, at the noon-dawn sector. In order to detect a prevalent pattern for the behavior of the geomagnetic-disturbance distribution, a statistical analysis was done by means of occurrence histograms, for different levels of the relative intensity of the storm as a function of local time. The relative intensity for each event was defined as a parameter varying between 0 and 1, with 0 (1) corresponding to the maximum (minimum) horizontal field disturbance during that particular event. Although this analysis does not show the temporal evolution of the disturbance, it confirms the above conclusions about its LT distribution. When only the main phases of the storms are considered in the statistics, the basic differences are the dawn peak is lightly shifted towards noon and that the noon-dawn contribution becomes larger. The observed distributions were tentatively associated with the corresponding interplanetary causes of the events. Since among the eight considered storms four are associated to magnetic cloud with a shock interplanetary structure (sMC) and three to sheath regions followed by a magnetic cloud (SH/MC), the statistical study was also performed for the two subsets of storms separately. For the first group (sMC) the LT distribution looks very similar to that of the whole set of storms. On the other hand, it was observed that for the last group (SH/MC) the peak around midnight was not present. This result might be a consequence that these type of storms are probably not associated to the presence of substorms.
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Chave SecundáriaINPE--PRE/
DOI10.1016/j.pss.2012.11.002
ISSN0032-0633
Chave de CitaçãoTsurutaniEchRicKoeGla:2013:DSOb
TítuloSLAMS at comet 19P/Borrelly: DS1 observations
Ano2013
Data de Acesso24 fev. 2021
Número de Arquivos1
Tamanho1808 KiB
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Autor1 Tsurutani, Bruce T.
2 Echer, Ezequiel
3 Richter, Ingo
4 Koenders, Christoph
5 Glassmeier, Karl-Heinz
Grupo1
2 DGE-CEA-INPE-MCTI-GOV-BR
Afiliação1 Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena 91109, CA, USA
2 Instituto Nacional de Pesquisas Espaciais (INPE)
3 Institut für Geophysik und Extraterrestrische Physik, Technische Universität Braunschweig, Braunschweig, Germany
4 Institut für Geophysik und Extraterrestrische Physik, Technische Universität Braunschweig, Braunschweig, Germany
5 Institut für Geophysik und Extraterrestrische Physik, Technische Universität Braunschweig, Braunschweig, Germany
RevistaPlanetary and Space Science
Volume75
Páginas17-27
Tipo SecundárioPRE PI
Nota SecundáriaB1_ASTRONOMIA_/_FÍSICA A2_GEOCIÊNCIAS B1_INTERDISCIPLINAR
Histórico2013-01-07 17:12:47 :: marciana -> administrator ::
2013-01-07 17:12:48 :: administrator -> marciana :: 2012
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Palavras-ChaveComet Borrelly, SLAMS, ion pickup, plasma waves.
ResumoComet 19P/Borrelly plasma waves associated with the ion pickup process are being studied for the first time. The compressive plasma waves (short, large-amplitude, magnetic structures, or SLAMS) have peak-to-background magnetic field magnitude amplitudes as large as ∼91. A new method of analysis has been developed to study the properties these compressive waves (and the bow shock) and is applied in this study. The bow shock at the time of the DS1 crossing was determined to be quasiparallel in nature with θBn∼22°. Using this new technique and minimum variance analyses over single wave cycles, most of the waves were determined to be circularly polarized, but some were noted to have linear and sunglass polarizations. The waves propagated obliquely to the ambient magnetic field B0, with over 75% of the cases with θkB0>45°. The intrinsic wave polarization in the plasma frame was investigated by examining waves propagating obliquely to the solar wind direction, θkx>75°, where x is the solar wind velocity vector. From this analysis, a mix of right-hand (RH) and left-hand (LH) polarization waves were found, with no particular order, either as a function of distance upstream or closeness to the bow shock. Most of the waves were detected when B0 was oblique to Vsw. The equal mix of RH and LH waves is not well explained by current theoretical models. It is possible that the Dubouloz and Scholer (1995) scenario could work for this cometary case if both RH and LH waves were generated by ring-beam distributions.
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Chave SecundáriaINPE--PRE/
DOI10.1016/j.asr.2012.03.006
ISSN0273-1177
Chave de CitaçãoSzajkoCrisMandDalL:2013:VeInGe
TítuloVery intense geomagnetic storms and their relation to interplanetary and solar active phenomena
ProjetoCNPq 303798/2008-4 and 481368/2010-8.
Ano2013
MêsMay
Data de Acesso24 fev. 2021
Número de Arquivos1
Tamanho1527 KiB
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Autor1 Szajko, N. S.
2 Cristiani, G.
3 Mandrini, C. H.
4 Dal Lago, Alisson
Identificador de Curriculo1
2
3
4 8JMKD3MGP5W/3C9JGH3
Grupo1
2
3
4 DGE-CEA-INPE-MCTI-GOV-BR
Afiliação1 Instituto de Astronomía y Física del Espacio, CONICET-UBA, Buenos Aires
2 Instituto de Astronomía y Física del Espacio, CONICET-UBA,Buenos Aires
3 Instituto de Astronomía y Física del Espacio, CONICET-UBA, 428 Buenos Aires
4 Instituto Nacional de Pesquisas Espaciais (INPE)
Endereço de e-Mail do Autor1 natisolsz@hotmail.com
2 gcristiani@iafe.uba.ar
3 mandrini@iafe.uba.ar
4 dallago@dge.inpe.br
Endereço de e-Mailtereza@sid.inpe.br
RevistaAdvances in Space Research
Volume51
Número10
Páginas1842-1856
Tipo SecundárioPRE PI
Nota SecundáriaB1 B1 B1 B1 B2 B3 B4
Histórico2012-08-07 14:08:32 :: tereza@sid.inpe.br -> administrator ::
2012-08-07 14:08:32 :: administrator -> tereza@sid.inpe.br :: 2012
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Palavras-ChaveVery intense geomagnetic storms, Solar activity, CMEs/ICMEs.
ResumoWe revisit previous studies in which the characteristics of the solar and interplanetary sources of intense geomagnetic storms have been discussed. In this particular analysis, using the Dst time series, we consider the very intense geomagnetic storms that occurred during Solar Cycle 23 by setting a value of as threshold. After carefully examining the set of available solar and in situ observations from instruments aboard the Solar and Heliospheric Observatory (SOHO) and the Advanced Composition Explorer (ACE), complemented with data from the ground, we have identified and characterized the solar and interplanetary sources of each storm. That is to say, we determine the time, angular width, plane-of-the-sky, lateral expansion, and radial velocities of the source coronal mass ejection (CME), the type and heliographic location of the CME solar source region (including the characteristics of the sunspot groups), and the time duration of the associated flare. After this, we investigate the overall characteristics of the interplanetary (IP) main-phase storm driver, including the time arrival of the shock/disturbance at 1 AU, the type of associated IP structure/ejecta, the origin of a prolonged and enhanced southward component (Bs) of the IP field, and other characteristics related to the energy injected into the magnetosphere during the storm (i.e. the solar wind maximum convected electric field, Ey). The analyzed set consists of 20 events, some of these are complex and present two or more Dst minima that are, in general, due to consecutive solar events. The 20 storms are distributed along Solar Cycle 23 (which is a double-peak cycle) in such a way that 15% occurs during the rising phase of the cycle, 45% during both cycle maxima, and, surprisingly, 40% during the cycle descending phase. This latter set includes half of the superstorms and the only cycle extreme event. 85% of the storms are associated to full halo CMEs and 10% to partial halo events. One of the storms occurred at the time contact with SOHO was lost. The CME solar sources of all analyzed storms, but one, are active regions (ARs). The source of the remaining CME is a bipolar low-field region where a long and curved filament erupts. The ARs where the CMEs originate show, in general, high magnetic complexity; ¦Ä spots are present in 74% of the ARs, 10% are formed by several bipolar sunspot groups, and only 16% present a single bipolar sunspot group. All CMEs are associated to long duration events (LDEs), exceeding 3 h in all cases, with around 75% lasting more than 5 h. The associated flares are, in general, intense events, classified as M or X in soft X-rays; only 3 of them fall in the C class, with the one happening in the bipolar low field region hardly reaching the C level. We calculate the lateral expansion velocity for most of the CMEs. The values found exceed in all cases but one the fast solar wind speed (¡Ö750 km s−1). The average lateral expansion velocity is 2400 km s−1. The spatial distribution of the solar CME sources on the solar disk shows an evident asymmetry; while there are no sources located more eastward than 12¡ã in longitude, there are 7 events more westward than12¡ã. Nevertheless, the bulk of the solar sources are located near Sun center, i.e. at less than 20¡ã in longitude or latitude. Considering the IP structures responsible for a long and enhanced Bs, we find that 35% correspond to magnetic clouds (MCs) or ICME fields, 30% to sheath fields, and 30% to combined sheath and MC or ICME fields. For only one storm the origin of Bs is related to the back compression of an ICME by a high speed stream coming from a coronal hole in the neighborhood of the corresponding CME source region. We have also found that for this particular set of storms the linear relation between Ey and the storm intensity holds (with a correlation coefficient of 0.73). These results complement and extend those of other works in the literature.
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DOI10.1051/swsc/2013048
ISSN2115-7251
Rótulolattes: 3368023405805386 11 SaizCCDHNSBDDGMTV:2013:GeReSo
Chave de CitaçãoSaizCCDHNSBDDGMTV:2013:GeReSo
TítuloGeomagnetic response to solar and interplanetary disturbances
Ano2013
Data de Acesso24 fev. 2021
Número de Arquivos1
Tamanho2510 KiB
Área de contextualização
Autor 1 Saiz, Elena
 2 Cerrato, Yolanda
 3 Cid, Consuelo
 4 Dobrica, Venera
 5 Hejda, Pavel
 6 Nenovski, Petko
 7 Stauning, Peter
 8 Bochnicek, Josef
 9 Danov, Dimitar
10 Demetrescu, Crisan
11 Gonzalez, Walter Demetrio
12 Maris, Georgeta
13 Teodosiev, Dimitar
14 Valach, Fridich
Identificador de Curriculo 1
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11 8JMKD3MGP5W/3C9JJC4
Grupo 1
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11 DGE-CEA-INPE-MCTI-GOV-BR
Afiliação 1 Space Research Group-Space Weather, Departamento de Fı´sica, Universidad de Alcala´, Madrid, Spain
 2 Institute of Geodynamics, Romanian Academy, Bucharest, Romania
 3 Institute of Geophysics of the ASCR, Prague, Czech Republic
 4 National Institute for Geophysics, Geodesy and Geography, Bulgarian Academy of Sciences, 1113 Sofia, Bulgaria
 5 Institute for Space Research and Technologies, Bulgarian Academy of Sciences, 1113 Sofia, Bulgaria
 6 National Institute for Geophysics, Geodesy and Geography, Bulgarian Academy of Sciences, 1113 Sofia, Bulgaria
 7 Danish Meteorological Institute, Copenhagen, Denmark
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 9 Institute for Space Research and Technologies, Bulgarian Academy of Sciences, 1113 Sofia, Bulgaria
10 Institute of Geodynamics, Romanian Academy, Bucharest, Romania
11 Instituto Nacional de Pesquisas Espaciais (INPE)
12 Institute of Geodynamics, Romanian Academy, Bucharest, Romania
13 Institute for Space Research and Technologies, Bulgarian Academy of Sciences, 1113 Sofia, Bulgaria
14 Geomagnetic Observatory, Geophysical Institute, Slovak Academy of Sciences, Hurbanovo, Slovakia
Endereço de e-Mail do Autor 1
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11 gonzalez@dge.inpe.br
Endereço de e-Mailgonzalez@dge.inpe.br
RevistaJournal of Space Weather and Space Climate
Volume3
PáginasA26
Tipo SecundárioPRE PI
Nota SecundáriaB5
Histórico2013-12-12 18:39:09 :: lattes -> administrator ::
2018-06-04 23:39:25 :: administrator -> marcelo.pazos@inpe.br :: 2013
Área de conteúdo e estrutura
É a matriz ou uma cópia?é a matriz
Estágio do Conteúdoconcluido
Transferível1
Tipo do ConteudoExternal Contribution
Tipo de Versãopublisher
Palavras-Chavesolar activity, interplanetary medium, indices, ionosphere (general), ring current.
ResumoThe space weather discipline involves different physical scenarios, which are characterised by very different physical conditions, ranging from the Sun to the terrestrial magnetosphere and ionosphere. Thanks to the great modelling effort made during the last years, a few Sun-to-ionosphere/thermosphere physics-based numerical codes have been developed. However, the success of the prediction is still far from achieving the desirable results and much more progress is needed. Some aspects involved in this progress concern both the technical progress (developing and validating tools to forecast, selecting the optimal parameters as inputs for the tools, improving accuracy in prediction with short lead time, etc.) and the scientific development, i.e., deeper understanding of the energy transfer process from the solar wind to the coupled magnetosphere-ionosphere-thermosphere system. The purpose of this paper is to collect the most relevant results related to these topics obtained during the COST Action ES0803. In an end-to-end forecasting scheme that uses an artificial neural network, we show that the forecasting results improve when gathering certain parameters, such as X-ray solar flares, Type II and/or Type IV radio emission and solar energetic particles enhancements as inputs for the algorithm. Regarding the solar wind-magnetosphere-ionosphere interaction topic, the geomagnetic responses at high and low latitudes are considered separately. At low latitudes, we present new insights into temporal evolution of the ring current, as seen by Burtons equation, in both main and recovery phases of the storm. At high latitudes, the PCC index appears as an achievement in modelling the coupling between the upper atmosphere and the solar wind, with a great potential for forecasting purposes. We also address the important role of small-scale field-aligned currents in Joule heating of the ionosphere even under non-disturbed conditions. Our scientific results in the framework of the COST Action ES0803 cover the topics from the short-term solar-activity evolution, i.e., space weather, to the long-term evolution of relevant solar/heliospheric/magnetospheric parameters, i.e., space climate. On the timescales of the Hale and Gleissberg cycles (22- and 88-year cycle respectively) we can highlight that the trend of solar, heliospheric and geomagnetic parameters shows the solar origin of the widely discussed increase in geomagnetic activity in the last century.
AreaCEA
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