Dynamical evolution of V-type photometric candidates in the outer main belt

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Huaman, M. E. [UNESP]
Carruba, V. [UNESP]
Domingos, R. C. [UNESP]

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Oxford Univ Press


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.



celestial mechanics, minor planets, asteroids: general

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Monthly Notices Of The Royal Astronomical Society. Oxford: Oxford Univ Press, v. 444, n. 3, p. 2985-2992, 2014.