| Full text | |
| Author(s): |
Total Authors: 3
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| Affiliation: | [1] Univ Estadual Paulista, UNESP, Grp Dinam Orbital & Planetol, BR-12516410 Guaratingueta, SP - Brazil
[2] Univ Estadual Paulista, UNESP, BR-13874149 Sao Joao Da Boa Vista, SP - Brazil
Total Affiliations: 2
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| Document type: | Journal article |
| Source: | Monthly Notices of the Royal Astronomical Society; v. 444, n. 3, p. 2985-2992, NOV 1 2014. |
| Web of Science Citations: | 7 |
| Abstract | |
V-type asteroids, characterized by two absorption bands at 1.0 and 2.0 mu m, are usually thought to be portions of the crust of differentiated or partially differentiated bodies. Most V-type asteroids are found in the inner main belt and are thought to be current or past members of the Vesta dynamical family. Recently, several V-type photometric candidates have been identified in the central and outer main belt. While the dynamical evolution of V-type photometric candidates in the central main belt has been recently investigated, less attention has been given to the orbital evolution of basaltic material in the outer main belt as a whole. Here, we identify known and new V-type photometric candidates in this region, and study their orbital evolution under the effect of gravitational and non-gravitational forces. A scenario in which a minimum of three local sources, possibly associated with the parent bodies of (349) Dembowska, (221) Eos, and (1459) Magnya, could in principle explain the current orbital distribution of V-type photometric candidates in the region. (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 |