@Article{AraujoMoraPradWint:2017:MaStDi,
author = "Araujo, Rosana Aparecida Nogueira de and Moraes, Rodolpho Vilhena
de and Prado, Antonio Fernando Bertachini de Almeida and Winter,
O. C.",
affiliation = "{Universidade Federal de S{\~a}o Paulo (UNIFESP)} and {Instituto
Nacional de Pesquisas Espaciais (INPE)} and {Instituto Nacional de
Pesquisas Espaciais (INPE)} and {Universidade Estadual Paulista
(UNESP)}",
title = "Mapping stable direct and retrograde orbits around the triple
system of asteroids (45) Eugenia",
journal = "Monthly Notices of the Royal Astronomical Society",
year = "2017",
volume = "472",
number = "4",
pages = "3999--4006",
month = "Dec.",
keywords = "methods: numerical, celestial mechanics, minor planets, asteroids:
individual: (45) Eugenia, planets and satellites: dynamical
evolution and stability.",
abstract = "It is widely accepted that knowing the composition and the orbital
evolution of asteroids might help us to understand the process of
formation of the Solar system. It is also known that asteroids can
represent a threat to our planet. Such an important role has made
space missions to asteroids a very popular topic in current
astrodynamics and astronomy studies. Taking into account the
increasing interest in space missions to asteroids, especially to
multiple systems, we present a study that aims to characterize the
stable and unstable regions around the triple system of asteroids
(45) Eugenia. The goal is to characterize the unstable and stable
regions of this system and to make a comparison with the system
2001 SN263, which is the target of the Advanced Spaceborne Thermal
Emission and Reflection Radiometer (ASTER) mission. A new concept
was used for mapping orbits, by considering the disturbance
received by the spacecraft from all perturbing forces
individually. This method has also been applied to (45) Eugenia.
We present the stable and unstable regions for particles with
relative inclination between 0° and 180°. We found that (45)
Eugenia presents larger stable regions for both prograde and
retrograde cases. This is mainly because the satellites of this
system are small when compared to the primary body, and because
they are not close to each other. We also present a comparison
between these two triple systems, and we discuss how these results
can guide us in the planning of future missions.",
doi = "10.1093/mnras/stx2230",
url = "http://dx.doi.org/10.1093/mnras/stx2230",
issn = "0035-8711 and 1365-2966",
language = "en",
targetfile = "araujo_mapping.pdf",
urlaccessdate = "27 abr. 2024"
}