Composition of the lunar surface as will be seen from SMART‐1: A simulation using Clementine data

Abstract

We present a new technique for remote sensing determination of lunar surface composition in the context of the SMART‐1 mission. The technique is based on spectral and composition data obtained by Lunar Soil Characterization Consortium for a few particle‐size separates of lunar soils. We map the abundance of TiO 2 and FeO, pyroxene content, maturity degree (I s /FeO), and a characteristic size of particles. Comparison of the TiO 2 and FeO abundance maps with proper distributions obtained by Lucey et al. [2000a] shows high correlation. We found also an inverse correlation between the I s /FeO distribution and Lucey et al. 's [2000b] parameter OM . Application of this approach shows that fresh mare crater regolith is characterized with a higher abundance of pyroxenes, coarse particles, and low maturity degree. The pyroxene abundance map can be used to identify pyroclastic regions. An excess of small particles is predicted for highland areas. We note appreciable variations of the characteristic size of particles in mare regions. Our preliminary results for the Reiner‐γ formation show that there is no composition anomaly for the TiO 2 and FeO abundance, in agreement with previous analyses. Our maps also indicate that the formation contains a surface material characterized with low maturity and high degree of crystallinity, consistent with the occurrence of immature regolith possibly contaminated with dust.