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Reference TypeThesis
Sitemtc-m16d.sid.inpe.br
Holder Codeisadg {BR SPINPE} ibi 8JMKD3MGPCW/3DT298S
Identifier8JMKD3MGP7W/36G6PES
Repositorysid.inpe.br/mtc-m19@80/2009/11.30.12.58
Last Update2010:04.20.16.19.28 (UTC) sergio
Metadatasid.inpe.br/mtc-m19@80/2009/11.30.12.58.18
Metadata Last Update2021:05.31.17.32.52 (UTC) sergio
Secondary KeyINPE-16649-TDI/1612
Citation KeySilva:2010:DeDiSo
TitleDetecção de distúrbios solar-interplanetários combinando observações de satélite e de raios cósmicos de superfície para aplicação em clima espacial
Alternate TitleSolar-interplanetary disturbances detection combining satellite and ground cosmic rays observations for space weather aplication
CourseGES-SPG-INPE-MCT-BR
Year2010
Date2009-12-18
Access Date2021, July 25
Thesis TypeTese (Doutorado em Geofísica Espacial)
Number of Pages140
Number of Files1
Size21058 KiB
Context area
AuthorSilva, Marlos Rockenbach da
GroupGES-SPG-INPE-MCT-BR
CommitteeMuralikrisna, Polinaya (presidente)
Dal Lago, Alisson (orientador)
Echer, Ezequiel
Alves, Maria Virgínia
Schuch, Nelson Jorge
Raulin, Jean-Pierre
Serbeto, Antonio de Padua Brito
e-Mail Addressmarlosrs@gmail.com
UniversityInstituto Nacional de Pesquisas Espaciais (INPE)
CitySão José dos Campos
Secondary TypeTDI
History (UTC)2009-11-30 12:58:19 :: marlosrs@gmail.com -> yolanda ::
2009-12-09 19:26:29 :: yolanda -> marlosrs@gmail.com ::
2010-02-03 11:13:57 :: marlosrs@gmail.com -> yolanda ::
2010-02-23 12:15:59 :: yolanda -> camila ::
2010-03-08 14:58:16 :: camila -> ricardo ::
2010-04-20 16:19:29 :: ricardo -> viveca@sid.inpe.br ::
2010-04-27 16:32:40 :: viveca@sid.inpe.br -> administrator ::
2018-08-14 15:15:20 :: administrator -> sergio :: 2010
Content and structure area
Is the master or a copy?is the master
Content Stagecompleted
Transferable1
Keywordstempestades geomagnéticas, raios cósmicos, estruturas solares, previsão de tempestades geomagnéticas, clima espacial, cosmic rays, geomagnetic storms, solar structures, geomagnetic storms prediction, space weather.
AbstractNesta tese é mostrada que a nova metodologia proposta para a análise dos dados da Rede de Muons, em operação desde 2001, passando a chamar-se Rede Global de Detectores de Muons (Global Muon Detector Network) - GMDN após 2006, pode ser uma importante ferramenta para a previsão de estruturas solares que causam tempestades geomagnéticas. Para isto foram utilizados dados registrados pelos instrumentos a bordo do satélite Advanced Composition Explorer - ACE, e dados de raios cósmicos de superfície dos telescópios que formam a GMDN no período de 2001 a 2007. Os telescópios cintiladores de muons encontram-se instalados no Observatório Espacial do Sul - OES/CRS/CIE/INPE-MCT em São Martinho da Serra, Brasil, Nagoya University em Nagoya, Japão, Australian Antartic Division - University of Tansmania em Hobart, Australia e Kuwait University no Kuwait. Os eventos foram classificados de acordo com a intensidade das tempestades medida pelo índice Dst, da seguinte forma: Tempestades Moderadas - MS (- 50 > Dst > -100), Tempestades Intensas - IS (-100 > Dst > -250) e Tempestades Superintensas - SS (Dst < -250). A nova metodologia foi comparada a metodologia de Munakata et al. (2000), sendo observado o dobro de precursores para os três tipos de tempestades com a metodologia proposta nesta tese. As tempestades superintensas são as de maior "previsibilidade", seguidas pelas tempestades intensas e a de menor observação de precursores são as tempestades moderadas. Também foi comprovada a melhoria da metodologia proposta nesta tese, tanto no número de precursores observados, quanto na qualidade de observação dos efeitos, em relação à metodologia de Munakata et al, (2000), e pela primeira vez, há indícios de precursores de tempestades causadas por regiões de interação corotantes (Corotating Interaction Region - CIR). ABSTRACT: In this thesis we show that the new methodology to analize data from the Muon Network in operation since 2001, being called Global Muon Detector Network - GMDN after 2006, can be considered an important tool for the forecasting of solar structures causing geomagnetic storms. Interplanetary and cosmic ray ground based data registered by the instruments onboard the Advanced Composition Explorer (ACE) satellite, and ground based cosmic rays detectors that compose the Muon Network were analyzed from 2001 to 2007. Four different muon cintillator telescopes were used for this study: one installed in the Southern Space Observatory - SSO/CRS/CIE/INPE-MCT, in São Martinho da Serra, Brazil; the other one in Nagoya University, in Nagoya, Japan; another one in the Australian Antartic Division - University of Tansmania in Hobart, Australia; and the last one in the Kuwait University in Kuwait City, Kuwait. The events analyzed were classified into three cathegories according to the storm intensity measured by the Dst index: Moderate Storms (MS) (-50 > Dst > -100 nT), Intense Storms (IS) (-100 > Dst > -250 nT), and Superstorms (SS) (Dst < -250 nT). The new methodology were compared with Munakata et al. (2000) methodology, where were observed that two times of precursors for that three kinds of storms were observed by the methodology proposed in this thesis. Super storms are the ones with the largest "previsibility", followed by the intense storms, and the smaller precursors observation are moderate storms. We could verify that the Proposed Methodology improved, as much in the number of observed precursors, as in the quality of the effects observed, compared to the Munakata et al, (2000)'s methodology, and for the first time, there is indication of precursors of geomagnetic storms caused by Corotating Interaction Region - CIR.
AreaCEA
Arrangementurlib.net > BDMCI > Fonds > Produção > GES > Detecção de distúrbios...
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@4primeirasPaginas_Marlos Rockenbach da Silva_16649.pdf 18/02/2010 13:37 154.8 KiB 
archive_last.zip 20/04/2010 10:54 96.3 MiB
FolhaAprovação.pdf 20/04/2010 10:48 33.9 KiB 
publicacao.pdf 20/04/2010 10:59 20.6 MiB
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zipped data URLhttp://urlib.net/zip/8JMKD3MGP7W/36G6PES
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Target Filepublicacao.pdf
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Mirror Repositorysid.inpe.br/mtc-m19@80/2009/08.21.17.02.53
Next Higher Units8JMKD3MGPCW/3F2PBEE
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