Dynamical lifetimes of near-Earth asteroids (NEAs) are shorter than the age of the Solar System thus necessitating resupply from the Main Belt. The NEA population, because of its proximity, allows us to explore asteroids at a size-range not possible among asteroids further away in the Main Belt. There are very few olivine-dominated asteroids, identified as spectroscopic A-types (Bus & Binzel 2002, DeMeo et al. 2009), among the near-Earth population (Binzel et al. 2004). While a number of NEAs were labeled olivine-rich from visible wavelength data, near-infrared observations of these objects prove the olivine-rich population is exceedingly rare. We identify (1951) Lick, (5261) Eureka, and a new third A-type object, (5131) 1990 BG. Using a radiative transfer model (Shkuratov et al. 1999) and band parameter analysis we mineralogically characterize and compare these three olivine-rich A-type asteroids. Additionally, using the model from Bottke et al. 2002, we present main-belt source regions for these bodies. Finally, we compare these NEA A-types to the main belt A-type population.
American Astronomical Society Meeting Abstracts #224
- Pub Date:
- June 2014