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

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

1 - 12 SHKURATOV ET AL.:

1 - 12 SHKURATOV ET AL.: COMPOSITION OF LUNAR SURFACE FROM SMART-1 maps. One example could be the Reiner-g formation. Our preliminary results confirm that this formation is not a chemical anomaly, at least in TiO 2 and FeO abundance, in agreement with previous analyses. Our maps also indicate that the formation contains a surface material with unusual properties characterized with low maturity and high degree of crystallinity, consistent with the occurrence of immature regolith possibly contaminated with dust. [56] 6. Our analysis and modeling with LSCC data and Clementine multispectral images show that SMART-1 multispectral data can be successfully used for estimating and mapping important parameters of the mare surface. However, data rate limitations for AMIE/SMART-1 do not allow obtaining a global image set for the Moon. This requires careful planning of sites to be imaged with the AMIE camera. Indeed, unusual areas, the regolith of which is perhaps not represented in the lunar sample collection, should be the most interesting. There are many examples of such areas, like swirls or red spots. On the other hand, our technique is developed using ‘‘ordinary’’ mare samples, and therefore our prediction is more reliable for typical mare regions. Thus prospective regions, which could be suggested for SMART-1 investigations, should include ‘‘standard’’ areas that are the Apollo and Luna landing sites. [57] Acknowledgments. This work is partially supported by INTAS grant 2000-0792, by the French Space Agency CNES, and by the Paul Sabatier University of Toulouse, with the attribution of visiting positions to VVS, YGS, and DGS. Research support from NASA grant NAG5-10469 (CMP) is gratefully acknowledged. This paper has also benefited from the preparatory work achieved by the AMIE/Smart-1 Science team. Authors thank D. Blewett for the thoughtful analysis of the paper. 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Keller, and D. S. McKay, Lunar mare soils: Space weathering and the major effects of surfacecorrelated nanophase Fe, J. Geophys. Res., 106, 27,985–28,000, 2001. Tompkins, S., and C. Pieters, Mineralogy of the lunar crust: Results from Clementine, Meteoritics Planet. Sci., 34, 25–41, 1999. Whitaker, E. A., Lunar color boundaries and their relationship to topographic features: A preliminary survey, Moon, 4, 348–355, 1972. B. Foing and Z. Sodnik, European Space Agency/European Space Research and Technology Center, Noordwijk, Netherlands. (bfoing@estec. esa.nl; Zoran.Sodnik@esa.int) J.-L. Josset, Jaquet-Droz 1, CSEM, CH-2007, Neuchâtel, Switzerland. ( jean-luc.josset@csem.ch) V. G. Kaydash, V. V. Omelchenko, Y. G. Shkuratov, and D. G. Stankevich, Astronomical Observatory of Kharkov National University, 35 Sumskaya St. Kharkov, 61022, Ukraine. (Yuriy_Shkuratov@hotmail.com; stankevich@ astron.kharkov.ua; vkaydash@astron.kharkov.ua; omelchenko@astron. kharkov.ua.) C. Pieters, Geological Sciences, Brown University, Providence, RI 02912, USA. ( pieters@mare.geo.brown.edu) P. Pinet, S. Chevrel, and Y. Daydou, University P. Sabatier Observatory Midi-Pyrenees, 14 Av. E. Belin, 31400 Toulouse, France. (Patrick.Pinet@ cnes.fr; Serge.Shevrel@cnes.fr; Yves.Daydou@cnes.fr) V. Shevchenko, Shternberg Astronomical Institute, Moscow, 119899, Russia. (Shev@sai.msu.ru) L. Taylor, Planetary Geoscience Institute, University of Tennessee, Knoxville, TN 37996, USA. (ltaylor@utk.edu)

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