Mapping stable direct and retrograde orbits around the triple system of asteroids (45) Eugenia
Araujo, R. A.N. [UNESP]
Moraes, R. V.
Prado, A. F.B.A.
Winter, O. C. [UNESP]
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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.
Celestial mechanics, Methods: numerical, Minor planets, asteroids: individual: (45) Eugenia, Planets and satellites: dynamical evolution and stability
Monthly Notices of the Royal Astronomical Society, v. 472, n. 4, p. 3999-4006, 2017.