@MastersThesis{Masago:2014:EsÓrRe,
author = "Masago, Bruna Yukiko Pinheiro Lopes",
title = "Estudo de {\'o}rbitas ressonantes no sistema triplo 2001sn263",
school = "Instituto Nacional de Pesquisas Espaciais (INPE)",
year = "2014",
address = "S{\~a}o Jos{\'e} dos Campos",
month = "2014-02-27",
keywords = "asteroide triplo 2001SN263, sonda espacial, ressonantes, problema
bi-liptico inclinado precessando, achatamento J2, triple asteroid
2001sn263, spacecraft, resonants, precessiong inclined bi
elliptical problem, flattening J2.",
abstract = "O asteroide triplo 2001SN\$_{263}\$ {\'e} um \emph{Near-Earth
Asteroid} (NEA). Em 2008, os cientistas do Observat{\'o}rio de
Arecibo (Porto Rico) fizeram v{\'a}rias observa{\c{c}}{\~o}es
desse asteroide e descobriram que n{\~a}o se tratava apenas de um
corpo {\'u}nico, mas sim de um sistema triplo. Os dois corpos
menores orbitam o objeto central. O sistema consiste de um corpo
central (Alfa) de 2,6 km de di{\^a}metro e dois corpos menores
(Beta e Gama) de 0,78 km e 0,58 km de di{\^a}metro,
respectivamente. No que diz respeito ao corpo central, Beta tem
semieixo maior de 16,63 km e um per{\'{\i}}odo de 6,23 dias, e
Gama tem semieixo maior de 3,80 km e um per{\'{\i}}odo de 0,69
dias. As {\'o}rbitas da sonda espacial que s{\~a}o ressonantes
com o per{\'{\i}}odo dos corpos menores s{\~a}o bastante
{\'u}teis, pois possuem a vantagem de gerarem v{\'a}rios
encontros sucessivos com esses corpos, dentro da din{\^a}mica
kepleriana, sem a necessidade de manobras orbitais. Apesar da
din{\^a}mica utilizada ser mais complexa, as {\'o}rbitas
ressonantes foram mantidas, por serem consideradas como um bom
ponto inicial para a busca de {\'o}rbitas com passagens
m{\'u}ltiplas pelos corpos menores. A proximidade da sonda com os
corpos {\'e} de fundamental import{\^a}ncia para a
observa{\c{c}}{\~a}o dos mesmos. Este trabalho aborda diversas
{\'o}rbitas para a sonda espacial em torno do corpo principal
(Alfa), com o objetivo de encontrar as {\'o}rbitas que mais se
aproximam dos corpos menores. No primeiro cen{\'a}rio, o corpo
secund{\'a}rio estudado ser{\'a} Beta. Isso implica que
ser{\~a}o buscadas {\'o}rbitas que ser{\~a}o ressonantes com a
{\'o}rbita desse corpo secund{\'a}rio. Esse cen{\'a}rio
ser{\'a} chamado de Alfa-Beta-Sonda. O segundo cen{\'a}rio
ser{\'a} testado usando Alfa-Gama-Sonda. Como sistema
din{\^a}mico ser{\'a} assumido que Beta e Gama descrevem
{\'o}rbitas keplerianas el{\'{\i}}pticas e n{\~a}o coplanares
em torno de Alfa, e que a sonda espacial {\'e} perturbada pela
for{\c{c}}a gravitacional dos tr{\^e}s corpos que comp{\~o}em o
sistema triplo mais o achatamento do corpo principal. Estes
cen{\'a}rios s{\~a}o analisados usando o Problema
Bi-El{\'{\i}}ptico Inclinado Precessando. {\'E} assumido um
sistema de refer{\^e}ncia centrado no corpo principal e com o
plano de refer{\^e}ncia sendo aquele que cont{\'e}m a
{\'o}rbita do segundo corpo em massa, aqui denominado de Beta. Os
corpos Beta e Gama s{\~a}o assumidos estarem em {\'o}rbitas
el{\'{\i}}pticas, sendo que a {\'o}rbita de Gama est{\'a}
inclinada em rela{\c{c}}{\~a}o ao plano de refer{\^e}ncia.
Al{\'e}m disso, essas {\'o}rbitas s{\~a}o assumidas estarem
precessando devido {\`a} presen{\c{c}}a do achatamento do corpo
principal (J\$_{2}\$). Sendo assim, o argumento do periapsis
\$(\omega)\$, a longitude do nodo ascendente \$(\Omega)\$ e
a longitude do periapsis \$(\varpi)\$ s{\~a}o
fun{\c{c}}{\~o}es do tempo. Este trabalho analisou {\'o}rbitas
para a sonda com passagens pr{\'o}ximas {\`a} Beta e depois
pr{\'o}ximas {\`a} Gama. A melhor solu{\c{c}}{\~a}o, com base
nos resultados aqui obtidos, {\'e} montar a miss{\~a}o como uma
s{\'e}rie de trechos ligados por manobras orbitais. Isso
implicaria na escolha de trechos excelentes para a
observa{\c{c}}{\~a}o de um ou dois dos tr{\^e}s corpos que
comp{\~o}em o sistema e utilizar propuls{\~a}o para mudar a
sonda de um trecho para outro, assim podendo observar com
qualidade todos os corpos pertencentes ao sistema. Os resultados
mostraram que {\'o}rbitas ideais, sem corre{\c{c}}{\~a}o
orbital, que permitam a explora{\c{c}}{\~a}o dos tr{\^e}s
corpos s{\~a}o dif{\'{\i}}ceis de serem encontradas. Existem
algumas solu{\c{c}}{\~o}es que fornecem op{\c{c}}{\~o}es de
encontros pr{\'o}ximos com os tr{\^e}s corpos, mas {\'e} sempre
necess{\'a}rio certo cuidado com passagens pr{\'o}ximas demais,
devido ao risco de colis{\~a}o. ABSTRACT: The triple asteroid
2001SN\$_{263}\$ is a Near-Earth Asteroid (NEA). In 2008,
scientists at the Arecibo Observatory (Puerto Rico) made several
observations of the asteroid and found that it was not just a one
body, but also a triple system. Two smaller bodies orbit the
central object. The complete system consists of a central body
(Alpha) ofwith 2.6 km in diameter and two smaller bodies (Beta and
Gamma) of with 0.78 km and 0.58 km in diameter, respectively. The
smaller bodies describe orbits around the more massive body. With
respect to the central body, the second body has semi-major axis
of 16.63 km and a period of 6.23 days, and the third body has
semi-major axis of 3.80 km and a period of 0.69 days. The orbits
of the spacecraft that are resonant with the period of the smaller
bodies are useful because they generate several successive
encounters with those bodies, under a keplerian dynamics, without
the need for orbital maneuvers. Even using a better dynamics, the
resonant orbits were used, because they generates good starting
trajectories. The proximity of the probe with the bodies is of
fundamental importance for the observation of the themsame. This
work studies various orbits that the spacecraft would be donemake
around the main body and even around the smaller bodies. As oneIn
the first study, first study, iit is considered as that the main
body of the triple asteroid is Alpha, Beta is the secondary body
and the third one is the spacecraft, whose mass is considered
negligible. This scenario is called by the {"}Alpha-Beta-Probe
Scenario{"}. As a second study, it is considered that Alpha isas
the main body of the asteroid Alphasystem, Gama is the secondary
and the probe is the third body, again with negligible mass. This
scenario is called {"}Alpha-Gama-Probe Scenario{"}. For the
dynamical system it is assumed that Beta and Gamma describe
Keplerian elliptical orbits. Their orbits are inclined around
Alphanot coplanar. It is considered that the gravitational forces
of the three bodies and the flatness of the main body perturb the
orbit of the spacecraft orbit. These scenarios are analyzed using
the Precessiong Inclined Bi-Elliptical problem. It is assumed a
reference system centered on the main body and that the reference
plane is the one that contains the orbit of the second body Beta.
The bodies Beta and Gamma are assumed to be in elliptical orbits,
with the orbit of Gamma inclined with respect to the reference
plane. Moreover, these orbits are assumed to precess due to the
flattening of the main body (J\$_{2}\$). Therefore, the argument
of periapsis \$(\omega)\$, the longitude of the ascending node
\$(\Omega)\$ and the longitude of periapsis \$(\varpi)\$ are
functions of time. For the spacecraft, its motion is governed by
the gravitational pull of the three bodies and the flattening of
the central body Alpha. This work analyzed orbits with close
approaches with the Beta and then with Gama. The best solution,
based on the results obtained here, is to build the mission as a
series of segments connected by orbital maneuvers. This would
imply in choosing some of the excellent orbits for observing one
or two of the three bodies that exist in the system and then to
use propulsion to change the probe from one orbit to another, thus
being able to observe with quality all bodies belonging to the
system.The results showed that ideal orbits, without orbital
correction, enabling the exploration of the three bodies are hard
to find. There are some solutions that provide close encounters
with the three bodyies, but you always need some care with too
close passages, due to the risk of collisions.",
committee = "Winter, Othon Cabo (presidente) and Prado, Antonio Fernando
Bertachini de Almeida (orientador) and Chiaradia, Ana Paula Marins
(orientadora) and Ara{\'u}jo, Rosana Aparecida Nogueira de",
englishtitle = "Estudies of resonant orbits around 2001sn 263 asteroid",
language = "pt",
ibi = "8JMKD3MGP5W34M/3G2CSP2",
url = "http://urlib.net/ibi/8JMKD3MGP5W34M/3G2CSP2",
targetfile = "publicacao.pdf",
urlaccessdate = "27 abr. 2024"
}