Carruba, V. [UNESP]Huaman, M. E. [UNESP]Domingos, R. C. [UNESP]Dos Santos, C. R. [UNESP]Souami, D.2014-12-032014-12-032014-04-01Monthly Notices Of The Royal Astronomical Society. Oxford: Oxford Univ Press, v. 439, n. 3, p. 3168-3179, 2014.0035-8711http://hdl.handle.net/11449/112112The origin of this large population of V-type objects is not well understood. Since it seems unlikely that Vestoids crossing the 3J:-1A mean-motion resonance with Jupiter could account for the whole population of V-type asteroids in the central and outer main belt, origin from local sources, such as the parent bodies of the Eunomia, and of the Merxia and Agnia asteroid families, has been proposed as an alternative mechanism.In this work, we investigated the dynamical evolution of the V-type photometric candidates in the central main belt, under the effect of gravitational and non-gravitational forces. Our results show that dynamical evolution from the parent bodies of the Eunomia and Merxia/Agnia families on time-scales of 2 Byr or more could be responsible for the current orbital location of most of the low-inclined V-type asteroids.3168-3179engcelestial mechanicsminor planetsasteroids: generalArtigo10.1093/mnras/stu192WOS:000334114900077Acesso restrito475070901604227666521690834643270000-0002-0516-0420