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@PhDThesis{MagalhŃes:2017:TeVaIo,
               author = "Magalh{\~a}es, Fab{\'{\i}}ola Pinho",
                title = "Temporal variability of the Io plasma torus inferred from 
                         ground-based [SII] emission observations",
               school = "Instituto Nacional de Pesquisas Espaciais (INPE)",
                 year = "2017",
              address = "S{\~a}o Jos{\'e} dos Campos",
                month = "2016-09-16",
             keywords = "volcanism, Io plasma torus, Jupiter, magnetosphere, 
                         magnetosphere-ionosphere coupling, vulcanismo, tor{\'o}ide de 
                         plasma de Io, J{\'u}piter, magnetosfera, acoplamento 
                         magnetosfera-ionosfera.",
             abstract = "Jupiter\${'}\$s magnetosphere is the largest one in the Solar 
                         System. It is a very complex system with several moons embedded, 
                         effects of planetary corotation and solar wind driven convection 
                         superposed, and several plasma physics processes occurring. 
                         Immersed within the magnetospheric plasma are the four Galilean 
                         moons which orbit around Jupiter. Io, the innermost of 
                         Jupiter\${'}\$s four Galilean moons, is the principal source of 
                         the magnetospheric plasma and responsible for nearly 1 ton/s of 
                         ions introduced into Jupiters magnetosphere. Io has intense and 
                         energetic volcanic activity. The sulfur and oxygen present in 
                         Io\${'}\$s tenuous atmosphere, spewed by volcanoes, escapes 
                         forming an extended neutral cloud around Io and Jupiter. 
                         Subsequently, by ionization and pickup ions, a ring of charged 
                         particles encircling Jupiter is created, forming the Io plasma 
                         torus. The Io plasma torus is composed mainly of sulfur and oxygen 
                         ions. Also via atmospheric escape, an extended neutral is formed, 
                         composed mainly of sodium. The torus is about 2 Jupiter radii 
                         (R\$_{J}\$ = 71,492 km) in width and is centered on Ios orbit 
                         around Jupiter at a distance of \$\sim\$ 5.9 R\$_{J}\$ . 
                         Considering this scenario, it is reasonable to expect that the Io 
                         plasma torus should be affected by changes in Io\${'}\$s 
                         volcanism. With that thought in mind, this thesis presents the 
                         analysis and results of the ground-based observations of the [SII] 
                         6731 ┼ emission lines from the Io plasma torus for the year 1997. 
                         The observations occurred at the McMath-Pierce Solar Telescope at 
                         Kitt Peak and the data is part of a collaboration established 
                         during this thesis. The plasma torus is most dense around 
                         Io\${'}\$s orbit and from the [SII] 6731 ┼ emission lines we 
                         were able to obtain the brightness of both ansae. By conducting 
                         the Lomb-Scargle peridiogram we tried to measure the system III 
                         and IV periodicities. Due to a problem with scattered light too 
                         close to the ansae position, the results showed an amount of noise 
                         that does not allow a precise location of system IV. The 
                         importance to identify the system IV is the hypothesis that it is 
                         related to material radial transport through the Io plasma torus. 
                         Interactions between Io and the Jovian environment, particularly 
                         the Io plasma torus, are unique and not well understood. With this 
                         thesis we aim to improve the understanding of this complex coupled 
                         system. RESUMO: J{\'u}piter {\'e} o planeta que apresenta a 
                         maior magnetosfera do Sistema Solar. Imerso no plasma da 
                         magnetosfera est{\~a}o as quatro maiores luas de J{\'u}piter, 
                         conhecidas como Galileanas. O sistema de J{\'u}piter {\'e} 
                         bastante complexo, principalmente devido {\`a}s 
                         intera{\c{c}}{\~o}es f{\'{\i}}sicas que o envolvem. Io, a lua 
                         mais interna das galileanas, {\'e} a principal fonte de plasma e 
                         a respons{\'a}vel por cerca de 1 ton/s de {\'{\i}}ons 
                         introduzidos na magnetosfera do planeta. Io apresenta uma 
                         atividade vulc{\^a}nica intensa e energ{\'e}tica, 
                         respons{\'a}vel por formar a atmosfera t{\^e}nue e n{\~a}o 
                         homog{\^e}nea de Io. Parte do material presente na atmosfera de 
                         Io escapa formando uma nuvem neutra em torno de Io e J{\'u}piter. 
                         Por ioniza{\c{c}}{\~a}o e troca de carga, um anel de 
                         part{\'{\i}}culas carregadas {\'e} formado ao redor de 
                         J{\'u}piter, formando o chamado tor{\'o}ide de plasma de Io. O 
                         tor{\'o}ide de plasma {\'e} composto principalmente de 
                         {\'{\i}}ons de enxofre e oxig{\^e}nio. Sua espessura {\'e} 
                         cerca de aproximadamente 2 raios de J{\'u}piter (R\$_{J}\$ = 
                         71,492 km) e est{\'a} centrada na {\'o}rbita de Io, a uma 
                         dist{\^a}ncia de \$\sim\$ 5,9 R\$_{J}\$ . O material 
                         observado em Io {\'e} o mesmo encontrado no tor{\'o}ide de 
                         plasma e por esta raz{\~a}o {\'e} razo{\'a}vel esperar que a 
                         intensa atividade vulc{\^a}nica de Io afete a variabilidade do 
                         tor{\'o}ide de plasma. A tese tem como objetivo apresentar 
                         an{\'a}lises e resultados provenientes de observa{\c{c}}{\~o}es 
                         obtidas da superf{\'{\i}}cie da Terra da linha de emiss{\~a}o 
                         do enxofre, na faixa do 6731 ┼ para o ano de 1997. As 
                         observa{\c{c}}{\~o}es ocorreram no telesc{\'o}pio Solar 
                         McMath-Pierce, localizado no Kitt Peak. A regi{\~a}o mais densa 
                         do tor{\'o}ide encontra-se em torno da {\'o}rbita de Io e a 
                         partir das observa{\c{c}}{\~o}es do enxofre ionizado {\'e} 
                         poss{\'{\i}}vel rastrear a parte mais densa do tor{\'o}ide e o 
                         brilho de cada \${''}\$ansa\${''}\$. A partir da medida dos 
                         brilhos {\'e} poss{\'{\i}}vel obter-se as periodicidades de 
                         J{\'u}piter. Para tal foi utilizado o periodograma de 
                         Lomb-Scargle. As intera{\c{c}}{\~o}es existentes entre Io e 
                         J{\'u}piter s{\~a}o {\'u}nicas e muito dos seus processos 
                         f{\'{\i}}sicos ainda n{\~a}o s{\~a}o compreendidos. Este 
                         trabalho tem como objetivo melhor compreender este sistema 
                         complexo acoplado.",
            committee = "Wrasse, Cristiano Max (presidente) and Alarcon, Walter 
                         Dem{\'e}trio Gonzalez (orientador) and Echer, Ezequiel 
                         (orientador) and Echer, Mariza Pereira de Souza (orientadora) and 
                         Fernandes, Francisco Carlos Rocha and Lopes, Rosaly Mutel Crocce 
                         and Morgenthaler, Jeffrey",
           copyholder = "SID/SCD",
         englishtitle = "Estudo da variabilidade temporal do tor{\'o}ide de plasma Io 
                         inferido a partir das emiss{\~o}es de [SII], de 
                         observa{\c{c}}{\~o}es da superf{\'{\i}}cie da Terra",
             language = "en",
                pages = "123",
                  ibi = "8JMKD3MGP3W34P/3MC5SSH",
                  url = "http://urlib.net/rep/8JMKD3MGP3W34P/3MC5SSH",
           targetfile = "publicacao.pdf",
        urlaccessdate = "03 dez. 2020"
}


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