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

TL;DR

This paper investigates the orbital evolution of V-type asteroids in the outer main belt, identifying potential source regions and analyzing their dynamical history under gravitational and non-gravitational influences.

Contribution

It extends the study of V-type asteroid evolution to the outer main belt, identifying candidates and proposing multiple local sources for their current distribution.

Findings

Multiple sources, including (349) Dembowska, (221) Eos, and (1459) Magnya, may explain the orbital distribution.

Orbital evolution influenced by gravitational and non-gravitational forces.

New V-type candidates identified in the outer main belt.

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.