@PhDThesis{Jauer:2014:EsSoRe,
author = "Jauer, Paulo Ricardo",
title = "Estudo sobre reconex{\~a}o magn{\'e}tica na magnetopausa
terrestre por meio de simula{\c{c}}{\~a}o MHD 3D BATS-R-US",
school = "Instituto Nacional de Pesquisas Espaciais (INPE)",
year = "2014",
address = "S{\~a}o Jos{\'e} dos Campos",
month = "2014-04-28",
keywords = "magnetosfera, magnetopausa, vento solar, simula{\c{c}}{\~a}o 3D
MHD, reconex{\~a}o magn{\'e}tica, magnetosphere, magnetopouse,
solar wind, MHD 3D simulation, magnetic reconnection.",
abstract = "A reconex{\~a}o magn{\'e}tica {\'e} um processo f{\'{\i}}sico
fundamental no contexto da intera{\c{c}}{\~a}o vento
solar-magnetosfera terrestre manifestando-se, por exemplo, na
din{\^a}mica dos fluxos de plasma na regi{\~a}o da magnetopausa
diurna e no conte{\'u}do energ{\'e}tico da magnetosfera. Neste
trabalho analisamos seus efeitos globais, para diferentes
orienta{\c{c}}{\~o}es do campo magn{\'e}tico
interplanet{\'a}rio (IMF) e par{\^a}metros do vento solar,
utilizando-se o modelo MHD 3D Global BATS-RUS. Na magnetopausa
observou-se que os fluxos de plasma deslocam-se perpendicularmente
{\`a} linha-X de reconex{\~a}o, quando o IMF {\'e} puramente
sul, \$B_{z}\$< O, ou possue, tamb{\'e}m, uma componente
\$B_{y}\$ n{\~a}o nula. Nas simula{\c{c}}{\~o}es a linha-X
localiza-se na regi{\~a}o equatorial quando \$B_{z}\$<O e
encontra-se rotacionada em rela{\c{c}}{\~a}o ao plano da
ecl{\'{\i}}ptica, no sentido anti-hor{\'a}rio e hor{\'a}rio,
respectivamente, para um campo interplanet{\'a}rio com
componentes (O, \$B_{y}\$ \$-B_{z}\$) e (O, \$-B_{y}\$,
\$-B_{z}\$). Estas orienta{\c{c}}{\~o}es foram confirmadas
atrav{\'e}s da aplica{\c{c}}{\~a}o do modelo de Gonzalez e
Mozer (1974). A compara{\c{c}}{\~a}o entre o padr{\~a}o dos
deslocamentos dos fluxos modelados pelo BATS-R-US e pelo modelo de
Cooling et aI. (2001) mostrou que estes diferem suas
trajet{\'o}rias nas regi{\~o}es dos flancos e altas latitudes.
Al{\'e}m disso, estimou-se a taxa de energia eletromagn{\'e}tica
em uma regi{\~a}o da magnetocauda, via integra{\c{c}}{\~a}o da
diverg{\^e}ncia do fluxo do vetor de Poynting. Os resultados
desta estimativa foram compilados em uma lista que consta de 22
eventos. Tais eventos revelam aspectos f{\'{\i}}sicos
fundamentais relacionados {\`a} intera{\c{c}}{\~a}o entre o
vento solar e a magnetosfera terrestre. Para um IMF-\$B_{z}\$
norte, independentemente \$B_{y}\$ > O ou \$B_{y}\$ < O, os
valores estimados da taxa de energia eletromagn{\'e}tica foram
semelhantes. Isso {\'e} verificado, tamb{\'e}m, quando o
IMF-\$B_{z}\$ {\'e} sul. No entanto, a taxa de energia {\'e}
diferente para os dois casos, sendo maior para \$B_{z}\$ sul.
Quando a magnitude do IMF-\$B_{z}\$ {\'e} aumentada de
-10\emph{nT} para -30\emph{nT}, observa-se um decr{\'e}scimo no
fluxo de energia eletromagn{\'e}tica. Isto ocorreu devido ao
dom{\'{\i}}nio da for{\c{c}}a magn{\'e}tica em
rela{\c{c}}{\~a}o ao gradiente de press{\~a}o na regi{\~a}o da
bainha magn{\'e}tica (Lopez et aI., 2010). Calculou-se,
tamb{\'e}m, a taxa de energia na magnetosfera para o evento de
tempestade magn{\'e}tica de 22-23 de setembro de 1999. Os
resultados mostraram que, durante o pico m{\'a}ximo da tempestade
magn{\'e}tica, a taxa de energia que penetrou a magnetocauda foi
de 2,89x\$10^{13}\$ W. Estes resultados foram comparados {\`a}
taxa de energia dissipada obtida com a equa{\c{c}}{\~a}o de
Akasofu (1981), que para esta tempestade foi de 1,63x\$10^{13}\$
W. Um balan{\c{c}}o energ{\'e}tico mostrou que 56\% desta
energia, {\'e} dissipada nas diferentes regi{\~o}es internas da
magnetosfera, enquanto os 44\% restantes s{\~a}o liberados
juntamente com plasm{\'o}ides. Os resultados obtidos pela
modelagem BATS-R-US concordam com aquele apresentado, por De Lucas
et aI. (2007), cujo valor foi de 2,97x\$10^{13}\$ W para esta
tempestade. Atrav{\'e}s da modelagem desta tempestade
geomagn{\'e}tica pode-se quantificar e testar a robustez e
precis{\~a}o da metodologia desenvolvida para o c{\'a}lculo da
penetra{\c{c}}{\~a}o do fluxo do vetor de Poynting para
regi{\~o}es internas da magnetocauda. ABSTRACT: The fundamental
physical process in the context of the solar windmagnetosphere
interaction is called magnetic reconnection. It plays an important
role on the dynamic of the dayside magnetopause plasma flows and
in the energy content of Earth 's magnetotail. In this study its
global effects were analyzed throughout different interplanetary
magnetic field (IMF) orientations and solar wind plasma parameters
simulations, performed by the 3D MHD global model BATS-R-US. At
the dayside magnetopause our results indicate that when IMF is
purely southward (\$B_{z}\$ < O) or has a non-zero \$B_{y}\$
component, the plasma flows move perpendicularly to the
reconnection X-line. The X-line, for a purely southward IMF, was
located at the equator. When a non-zero \$B_{y}\$ component was
added the X-line rotated relative to the plane of the ecliptic, in
a counterclockwise sense for \$B_{y}\$ > O, and in a clockwise
sense for \$B_{y}\$ < O. The BATS-R-US X-line's location and
orientation have been verified by applying the analytical model of
Gonzalez and Mozer (1974). The electromagnetic energy rate, within
a domain located at the tail, was also estimated by the
integration of the Poynting vector divergence. The results were
gathered in a list of 22 events. This list revealed fundamental
physical aspects regarding the solar wind-magnetosphere
interaction. We have found that the electromagnetic energy rate,
in the magnetotail, for a due northward and duskward IMF
orientation was similar to that of a due northward and dawnward
IMF. The same behavior is verified for a southward IMF
\$B_{z}\$, however, larger in this case. We have also simulated
the magnetospheric response to a gradual increase in the magnitude
of the due southward IMF (\$B_{z}\$) component (from -10 to -30
\emph{nT}). The energy rate was sustained when \$B_{z}\$
decreased from -10 to -15 \emph{nT}. However, when the
\$B_{z}\$ decreased from -20 to -30 \emph{nT} the energy has
also decreased. This was due to the enhanced magnetic field
strength at the magnetosheath region in relation to pressure
gradient (Lopez et aI., 2010). We have, also, modeled the main
phase of the September 22-23, 1999 geomagnetic storm. To which we
have estimated the energy rate at the tail in 2,89x\$10^{13}\$
W, during the peak of the storm. This result was compared to the
amount of the energy dissipated in the magnetosphere for the storm
obtained by the empirical equation derived by Akasofu (1981):
1,63x\$10^{13}\$ W. Our comparison indicated that 56\% of this
energy rate was dissipated in different regions of the inner
Earths magnetosphere, whereas the remaining 44\% was assumed to
be released along with plasmoids. The results obtained with the
BATS-R-US simulation agree with that presented by De lucas et aI.
(2007) whose estimated energy input value was 2,97x\$10^{13}\$ W
for this storm. By modeling an actual geomagnetic storm event we
could quantify and test the robustness and accuracy of the
methodology developed for the calculation of the penetration of
the Poynting vector flows to the inner regions of the Earths
magnetotail.",
committee = "Batista, Inez Staciarini (presidente) and Alarcon, Walter Demetrio
Gonzalez (orientador) and Costa, Cristiane Loesch de Souza
(orientadora) and Souza, Jonas Rodrigues de and Alves, Maria
Virg{\'{\i}}nia and Lucas, Aline de and Sim{\~o}es Junior,
Fernando Jaques Ruiz",
englishtitle = "Earth´s magnetopause magnetic reconnection study through a 3D MHD
BATS-R-US simulation",
language = "pt",
pages = "181",
ibi = "8JMKD3MGP5W34M/3G66A85",
url = "http://urlib.net/ibi/8JMKD3MGP5W34M/3G66A85",
targetfile = "publicacao.pdf",
urlaccessdate = "27 abr. 2024"
}