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dc.contributor.authorChanut, T. G. G. [UNESP]
dc.contributor.authorWinter, O. C. [UNESP]
dc.contributor.authorTsuchida, M. [UNESP]
dc.date.accessioned2014-12-03T13:11:07Z
dc.date.available2014-12-03T13:11:07Z
dc.date.issued2014-03-01
dc.identifierhttp://dx.doi.org/10.1093/mnras/stt2383
dc.identifier.citationMonthly Notices Of The Royal Astronomical Society. Oxford: Oxford Univ Press, v. 438, n. 3, p. 2672-2682, 2014.
dc.identifier.issn0035-8711
dc.identifier.urihttp://hdl.handle.net/11449/112881
dc.description.abstractOne of the techniques used in the past decade to determine the shape with a good accuracy and estimate certain physical features (volume, mass, moments of inertia) of asteroids is the polyhedral model method. We rebuild the shape of the asteroid 433 Eros using data from 1998 December observations of the probe Near-Earth-Asteroid-Rendezvous-Shoemaker. In our computations, we use a code that avoids singularities from the line integrals of a homogeneous arbitrary shaped polyhedral source. This code evaluates the gravitational potential function and its first- and second-order derivatives. Taking the rotation of asteroid 433 Eros into consideration, the aim of this work is to analyse the dynamics of numerical simulations of 3D initially equatorial orbits near the body. We find that the minimum radius for direct, equatorial circular orbits that cannot impact with the Eros surface is 36 km and the minimum radius for stable orbits is 31 km despite significant perturbations of its orbit. Moreover, as the orbits suffer less perturbations due to the irregular gravitational potential of Eros in the elliptic case, the most significant result of the analysis is that stable orbits exist at a periapsis radius of 29 km for initial eccentricities e(i) <= 0.2.en
dc.description.sponsorshipCoordenação de Aperfeiçoamento de Pessoal de Nível Superior (CAPES)
dc.description.sponsorshipConselho Nacional de Desenvolvimento Científico e Tecnológico (CNPq)
dc.description.sponsorshipINCT - Estudos do Espaco
dc.description.sponsorshipFundação de Amparo à Pesquisa do Estado de São Paulo (FAPESP)
dc.format.extent2672-2682
dc.language.isoeng
dc.publisherOxford University Press
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society
dc.sourceWeb of Science
dc.subjectgravitationen
dc.subjectmethods: numericalen
dc.subjectcelestial mechanicsen
dc.subjectminor planetsen
dc.subjectasteroids: individual: 433 Erosen
dc.title3D stability orbits close to 433 Eros using an effective polyhedral model methoden
dc.typeArtigo
dcterms.licensehttp://www.oxfordjournals.org/access_purchase/self-archiving_policyb.html
dcterms.rightsHolderOxford Univ Press
dc.contributor.institutionUniversidade Estadual Paulista (Unesp)
dc.description.affiliationUniv Estadual Paulista UNESP, Grp Dinam Orbital & Planetol, BR-12516410 Guaratingueta, SP, Brazil
dc.description.affiliationUniv Estadual Paulista UNESP, DCCE IBILCE, BR-15054000 Sao Jose Do Rio Preto, SP, Brazil
dc.description.affiliationUnespUniv Estadual Paulista UNESP, Grp Dinam Orbital & Planetol, BR-12516410 Guaratingueta, SP, Brazil
dc.description.affiliationUnespUniv Estadual Paulista UNESP, DCCE IBILCE, BR-15054000 Sao Jose Do Rio Preto, SP, Brazil
dc.identifier.doi10.1093/mnras/stt2383
dc.identifier.wosWOS:000331877000053
dc.rights.accessRightsAcesso restrito
dc.description.sponsorshipIdFAPESP: 11/08171-3
unesp.campusUniversidade Estadual Paulista (Unesp), Instituto de Biociências Letras e Ciências Exatas, São José do Rio Pretopt
dc.identifier.lattes3560557415176717
unesp.author.lattes3560557415176717
unesp.author.orcid0000-0002-8861-479X[1]
unesp.author.orcid0000-0002-4901-3289[2]
dc.relation.ispartofjcr5.194
dc.relation.ispartofsjr2,346
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