Chaotic diffusion caused by close encounters with several massive asteroids: II. the regions of (10) Hygiea, (2) Pallas, and (31) Euphrosyne

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dc.contributor.authorCarruba, V. [UNESP]
dc.contributor.authorHuaman, M. [UNESP]
dc.contributor.authorDomingos, R. C.
dc.contributor.authorRoig, F.
dc.contributor.institutionUniversidade Estadual Paulista (Unesp)
dc.contributor.institutionInstituto Nacional de Pesquisas Espaciais (INPE)
dc.contributor.institutionObservatório Nacional
dc.date.accessioned2014-05-27T11:28:23Z
dc.date.available2014-05-27T11:28:23Z
dc.date.issued2013-02-11
dc.description.abstractContext. Close encounters with (1) Ceres and (4) Vesta, the two most massive bodies in the main belt, are known to be a mechanism of dynamical mobility able to significantly alter proper elements of minor bodies, and they are the main source of dynamical mobility for medium-sized and large asteroids (D > 20 km, approximately). Recently, it has been shown that drift rates caused by close encounters with massive asteroids may change significantly on timescales of 30 Myr when different models (i.e., different numbers of massive asteroids) are considered. Aims. So far, not much attention has been given to the case of diffusion caused by the other most massive bodies in the main belt: (2) Pallas, (10) Hygiea, and (31) Euphrosyne, the third, fourth, and one of the most massive highly inclined asteroids in the main belt, respectively. Since (2) Pallas is a highly inclined object, relative velocities at encounter with other asteroids tend to be high and changes in proper elements are therefore relatively small. It was thus believed that the scattering effect caused by highly inclined objects in general should be small. Can diffusion by close encounters with these asteroids be a significant mechanism of long-term dynamical mobility? Methods. By performing simulations with symplectic integrators, we studied the problem of scattering caused by close encounters with (2) Pallas, (10) Hygiea, and (31) Euphrosyne when only the massive asteroids (and the eight planets) are considered, and the other massive main belt asteroids and non-gravitational forces are also accounted for. Results. By finding relatively small values of drift rates for (2) Pallas, we confirm that orbital scattering by this highly inclined object is indeed a minor effect. Unexpectedly, however, we obtained values of drift rates for changes in proper semi-major axis a caused by (10) Hygiea and (31) Euphrosyne larger than what was previously found for scattering by (4) Vesta. These high rates may have repercussions on the orbital evolution and age estimate of their respective families. © 2013 ESO.en
dc.description.affiliationUNESP Univ. Estadual Paulista Grupo de Dinâmica Orbital e Planetologia, Guaratinguetá, SP, 12516-410
dc.description.affiliationINPE Instituto Nacional de Pesquisas Espaciais, São José Dos Campos SP, 12227-010
dc.description.affiliationON Observatório Nacional, Rio de Janeiro, RJ, 20921-400
dc.description.affiliationUnespUNESP Univ. Estadual Paulista Grupo de Dinâmica Orbital e Planetologia, Guaratinguetá, SP, 12516-410
dc.identifierhttp://dx.doi.org/10.1051/0004-6361/201220448
dc.identifier.citationAstronomy and Astrophysics, v. 550.
dc.identifier.doi10.1051/0004-6361/201220448
dc.identifier.file2-s2.0-84873348984.pdf
dc.identifier.issn0004-6361
dc.identifier.issn1432-0746
dc.identifier.lattes4750709016042276
dc.identifier.lattes6652169083464327
dc.identifier.orcid0000-0002-0516-0420
dc.identifier.scopus2-s2.0-84873348984
dc.identifier.urihttp://hdl.handle.net/11449/74580
dc.identifier.wosWOS:000314879700085
dc.language.isoeng
dc.relation.ispartofAstronomy and Astrophysics
dc.relation.ispartofjcr5.565
dc.relation.ispartofsjr2,265
dc.relation.ispartofsjr2,265
dc.rights.accessRightsAcesso restrito
dc.sourceScopus
dc.subjectCelestial mechanics
dc.subjectMinor planets, asteroids: general
dc.subjectMinor planets, asteroids: individual: (10) Hygiea
dc.subjectMinor planets, asteroids: individual: (2) Pallas
dc.subjectMinor planets, asteroids: individual: (31) Euphrosyne
dc.subjectChaotic diffusion
dc.subjectDrift rates
dc.subjectHigh rate
dc.subjectMinor bodies
dc.subjectMinor planets , asteroids
dc.subjectMinor planets , asteroids: generals
dc.subjectNon-gravitational force
dc.subjectOrbital evolutions
dc.subjectRelative velocity
dc.subjectScattering effects
dc.subjectSemimajor axis
dc.subjectSignificant mechanism
dc.subjectSymplectic integrators
dc.subjectTime-scales
dc.subjectAstrophysics
dc.subjectDiffusion
dc.subjectScattering
dc.subjectAsteroids
dc.titleChaotic diffusion caused by close encounters with several massive asteroids: II. the regions of (10) Hygiea, (2) Pallas, and (31) Euphrosyneen
dc.typeArtigo
dcterms.licensehttp://www.aanda.org/index.php?option=com_content&view=article&id=902&Itemid=298
unesp.author.lattes4750709016042276
unesp.author.lattes6652169083464327[3]
unesp.author.orcid0000-0002-0516-0420[3]
unesp.campusUniversidade Estadual Paulista (Unesp), Faculdade de Engenharia, Guaratinguetápt
unesp.departmentMatemática - FEGpt

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