@PhDThesis{Magalhães: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 Å 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 Å 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 Å 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/ibi/8JMKD3MGP3W34P/3MC5SSH",
targetfile = "publicacao.pdf",
urlaccessdate = "27 abr. 2024"
}