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Composition of the lunar surface as will be seen ... - ResearchGate

Composition of the lunar surface as will be seen ... - ResearchGate

Composition of the lunar surface as will be seen ... -

JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 108, NO. E4, 5020, doi:10.1029/2002JE001971, 2003 Composition of the lunar surface as will be seen from SMART-1: A simulation using Clementine data Yuriy G. Shkuratov, 1 Dmitriy G. Stankevich, 1 Vadim G. Kaydash, 1 Vitaliy V. Omelchenko, 1 Carle M. Pieters, 2 Patrick C. Pinet, 3 Serge D. Chevrel, 3 Yves H. Daydou, 3 Bernard H. Foing, 4 Zoran Sodnik, 4 Jean-Luc Josset, 5 Lawrence A. Taylor, 6 and Vladislav V. Shevchenko 7 Received 23 August 2002; revised 21 January 2003; accepted 20 February 2003; published 3 April 2003. [1] 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-g 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. INDEX TERMS: 6250 Planetology: Solar System Objects: Moon (1221); 5420 Planetology: Solid Surface Planets: Impact phenomena (includes cratering); 5464 Planetology: Solid Surface Planets: Remote sensing; 5470 Planetology: Solid Surface Planets: Surface materials and properties; KEYWORDS: chemistry and mineralogy of the lunar surface Citation: Shkuratov, Y. G., et al., Composition of the lunar surface as will be seen from SMART-1: A simulation using Clementine data, J. Geophys. Res., 108(E4), 5020, doi:10.1029/2002JE001971, 2003. 1. Introduction [2] Multispectral photometry is a powerful tool to examine lunar surface chemistry, mineralogy, and physical properties. Pioneers of quantitative lunar spectral studies [e. g., Whitaker, 1972; McCord and Adams, 1973; Charette et al., 1974; McCord et al., 1976, 1981] clearly demonstrated the diagnostic potential of spectral reflectance measurements for the lunar surface. Multispectral photometric imaging 1 Kharkov Astronomical Observatory, Kharkov, Ukraine. 2 Geological Sciences, Brown University, Providence, Rhode Island, USA. 3 University P. Sabatier Observatoire Midi-Pyrenees, Toulouse, France. 4 European Space Agency/European Space Research and Technology Center, Noordwijk, Netherlands. 5 Cenre Suisse d’Electronique et de Microtechnique (CSEM), Neuchâtel, Switzerland. 6 Planetary Geoscience Institute, University of Tennessee, Knoxville, Tennessee, USA. 7 Shternberg Astronomical Institute, Moscow, Russia. Copyright 2003 by the American Geophysical Union. 0148-0227/03/2002JE001971$09.00 gives valuable information about the first few millimeters of the lunar regolith and provides the highest spatial resolution among remote sensing methods. Such data are very important for geologic studies of the lunar surface. [3] In 1994 the NASA-DoD Clementine spacecraft acquired multispectral images for more than 90% of the lunar surface [Nozette et al., 1994]. In fact, Clementine has opened a new era in geologic studies of the Moon with multispectral images of high spatial resolution. It allows considerable advance in understanding the history and evolution processes on the lunar surface [e.g., McEwen et al., 1994; Pieters et al., 1994; Shoemaker et al., 1994; Tompkins and Pieters, 1999; Blewett et al., 1997; Lucey et al., 1998, 2000a, 2000b; Le Mouelic et al., 2000; Pinet et al., 2000]. Multispectral Clementine data in combination with Earth-based observations and laboratory measurements of lunar samples allowed progress in evaluating the chemical composition of the lunar surface. The most widely used approach to estimate composition (TiO 2 , FeO), and maturity degree of the lunar surface was suggested by Lucey et al. [1995, 1998, 2000a, 2000b] and Blewett et al. [1997]. However, attempts to improve this algorithm or develop 1 - 1

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