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

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dc.citation.issue4
dc.citation.volume472
dc.contributor.authorAraujo, R. A. N. [UNIFESP]
dc.contributor.authorMoraes, R. V. [UNIFESP]
dc.contributor.authorPrado, A. F. B. A.
dc.contributor.authorWinter, O. C.
dc.coverageOxford
dc.date.accessioned2020-09-01T13:21:13Z
dc.date.available2020-09-01T13:21:13Z
dc.date.issued2017
dc.description.abstractIt 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.en
dc.description.affiliationNatl Inst Space Res INPE, BR-12201970 Sao Jose Dos Campos, SP, Brazil
dc.description.affiliationFed Univ Sao Paulo UNIFESP, ICT, BR-12247014 Sao Jose Dos Campos, SP, Brazil
dc.description.affiliationUniv Estadual Paulista UNESP, Grp Dinam Orbital & Planetol, BR-12516410 Guaratingueta, SP, Brazil
dc.description.affiliationUnifespFed Univ Sao Paulo UNIFESP, ICT, BR-12247014 Sao Jose Dos Campos, SP, Brazil
dc.description.sourceWeb of Science
dc.description.sponsorshipCNPq
dc.description.sponsorshipFAPESP
dc.description.sponsorshipIDCNPq: 150378/2015-7
dc.description.sponsorshipIDCNPq: 301338/2016-7
dc.description.sponsorshipIDFAPESP: 2016/24561-0
dc.description.sponsorshipIDFAPESP: 2011/08171-3
dc.format.extent3999-4006
dc.identifierhttp://dx.doi.org/10.1093/mnras/stx2230
dc.identifier.citationMonthly Notices Of The Royal Astronomical Society. Oxford, v. 472, n. 4, p. 3999-4006, 2017.
dc.identifier.doi10.1093/mnras/stx2230
dc.identifier.issn0035-8711
dc.identifier.urihttps://repositorio.unifesp.br/handle/11600/58131
dc.identifier.wosWOS:000415652500018
dc.language.isoeng
dc.publisherOxford Univ Press
dc.relation.ispartofMonthly Notices Of The Royal Astronomical Society
dc.rightsinfo:eu-repo/semantics/restrictedAccess
dc.subjectmethods: numericalen
dc.subjectcelestial mechanicsen
dc.subjectminor planets, asteroids: individual: (45) Eugeniaen
dc.subjectplanets and satellites: dynamical evolution and stabilityen
dc.titleMapping stable direct and retrograde orbits around the triple system of asteroids (45) Eugeniaen
dc.typeinfo:eu-repo/semantics/article
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