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• W1982643329 abstract "Multispectral data obtained by the Clementine mission are correlated to compositional and petrographic information for individual sample stations at the Apollo 17 landing site. The soils contain a variety of Fe 2+ ‐bearing phases in different proportions, including low‐ and high‐Ca pyroxene, olivine, ilmenite, and glass. In the mare soils, ilmenite carries a substantial proportion of the Fe 2+ , and in all soils, glasses, particularly agglutinates, carry nearly as much or more Fe 2+ as the silicates. Using an empirical calibration, concentrations of FeO and TiO 2 estimated from the ultraviolet‐visible (UVVIS) data correlate well with measured compositions of surface soils, yielding correlation coefficients of 0.94 and 0.95, respectively. The ferrous absorption, however, is weak in the mostly submature to mature Apollo 17 soils, thus spectral curvature is useful only for investigating the mafic‐silicate mineralogy around fresh craters and deposits. The effects of local topography cause significant variations in FeO and TiO 2 derived from Clementine UVVIS data but do not impair first‐order geologic interpretations. Parameters derived from the UVVIS data allow quantification of the composition and nature of the soils and, by inference, underlying rock formations and are consistent with the known geologic character of the landing site. The highland regions along this part of the Serenitatis rim are relatively FeO rich, partly as a result of abundant, mafic impact‐melt breccia and partly from the addition of basaltic material in the form of impact debris and pyroclastic deposits. At high elevations, massif soils are rich in a mafic melt‐breccia component, although slopes and areas mixed by small craters reveal a mixture of melt breccia and older highland material of anorthositic‐norite composition. Soils developed on hummocky deposits that postdate the massifs, such as the Sculptured Hills, have a similar range of compositions as the massifs. Elevated plains northeast of the Sculptured Hills are more mafic than the known impact‐melt breccias, suggesting that they may also contain an older volcanic component. Sources of low‐Ti basalt or very low Ti basalt, though not present in the immediate vicinity of the landing site, occur east and northeast of Taurus‐Littrow Valley and are readily identified using the UVVIS data." @default.
• W1982643329 created "2016-06-24" @default.
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• W1982643329 date "1999-06-01" @default.
• W1982643329 modified "2023-09-30" @default.
• W1982643329 title "Clementine UVVIS multispectral data and the Apollo 17 landing site: What can we tell and how well?" @default.
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• W1982643329 doi "https://doi.org/10.1029/1999je900012" @default.
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