Abstract
This chapter gives an outline of methods for describing the lunar surface in terms of specific spectral parameters inferred from multispectral or hyperspectral image data. These allow for the detection of specific lunar minerals, an estimation of the abundances of important chemical elements, and a mapping of the lunar surface in terms of its basic petrographic constituents.
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The compositions of the endmembers used to construct the petrographic maps in Fig. 3.8 are 18.0 wt% Fe, 6.5 wt% Mg, 6.9 wt% Al for mare basalt; 4.0 wt% Fe, 13.0 wt% Mg, 11.0 wt% Al for Mg-rich rock; and 0.5 wt% Fe, 1.0 wt% Mg, 17.0 wt% Al for FAN.
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The compositions of the basaltic endmembers used in Fig. 3.9b are 6.3 wt% Al and 3.6 wt% Ti for high-Ti basalt, 9.25 wt% Al and 1.6 wt% Ti for low-Ti basalt, and 14 wt% Al and 0.5 wt% Ti for high-Al basalt. High-Al basalts are described e.g. by Kramer et al. (2009).
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© 2013 Springer-Verlag Italia
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Lena, R., Wöhler, C., Phillips, J., Chiocchetta, M. (2013). Determination of Spectral Properties. In: Lunar Domes. Springer Praxis Books(). Springer, Milano. https://doi.org/10.1007/978-88-470-2637-7_3
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DOI: https://doi.org/10.1007/978-88-470-2637-7_3
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