| Full text | |
| Author(s): |
Carruba, V.
[1]
;
Huaman, M. E.
[1]
;
Domingos, R. C.
[1, 2]
;
Dos Santos, C. R.
[1]
;
Souami, D.
[3, 4, 5]
Total Authors: 5
|
| Affiliation: | [1] Univ Estadual Paulista, UNESP, Grp Dinam Orbital & Planetol, BR-12516410 Guaratingueta, SP - Brazil
[2] Inst Nacl Pesquisas Espaciais, BR-12227010 So Jos Dos Campos, SP - Brazil
[3] Univ Namur, Dept Math, Namur Ctr Complex Syst, NAXYS, B-5000 Namur - Belgium
[4] Univ Paris 06, F-75005 Paris - France
[5] Univ Paris 06, CNRS, UMR 8630, Observ Paris, SYRTE, F-75005 Paris - France
Total Affiliations: 5
|
| Document type: | Journal article |
| Source: | Monthly Notices of the Royal Astronomical Society; v. 439, n. 3, p. 3168-3179, APR 2014. |
| Web of Science Citations: | 17 |
| Abstract | |
The 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. (AU) | |
| FAPESP's process: | 11/19863-3 - Orbital mobility caused by close encounters with more than one massive asteroid |
| Grantee: | Valerio Carruba |
| Support Opportunities: | Regular Research Grants |