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(Reference retrieved automatically from Web of Science through information on FAPESP grant and its corresponding number as mentioned in the publication by the authors.)

Mapping stable direct and retrograde orbits around the triple system of asteroids (45) Eugenia

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Author(s):
Araujo, R. A. N. [1, 2, 3] ; Moraes, R. V. [3] ; Prado, A. F. B. A. [1] ; Winter, O. C. [2]
Total Authors: 4
Affiliation:
[1] Natl Inst Space Res INPE, BR-12201970 Sao Jose Dos Campos, SP - Brazil
[2] Univ Estadual Paulista UNESP, Grp Dinam Orbital & Planetol, BR-12516410 Guaratingueta, SP - Brazil
[3] Fed Univ Sao Paulo UNIFESP, ICT, BR-12247014 Sao Jose Dos Campos, SP - Brazil
Total Affiliations: 3
Document type: Journal article
Source: Monthly Notices of the Royal Astronomical Society; v. 472, n. 4, p. 3999-4006, DEC 2017.
Web of Science Citations: 0
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 degrees and 180 degrees. 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. (AU)

FAPESP's process: 11/08171-3 - Orbital dynamics of minor bodies
Grantee:Othon Cabo Winter
Support type: Research Projects - Thematic Grants
FAPESP's process: 16/24561-0 - On the relevance of small bodies in orbital dynamics
Grantee:Othon Cabo Winter
Support type: Research Projects - Thematic Grants