| Abstract: | Clementine ultraviolet-visible (UVVIS) data are used to examine the compositions of 18 pyroclastic deposits (15 small, three large) at 13 sites on the Moon. Compositional variations among pyroclastic deposits largely result from differing amounts of new basaltic (or juvenile) material and reworked local material entrained in their ejecta upon eruption. Characterization of pyroclastic deposit compositions allows us to understand the mechanisms of lunar explosive volcanism. Evidence for compositional differences between small pyroclastic deposits at a single site is observed at Atlas crater. At all sites, compositional variation among the small pyroclastic deposits is consistent with earlier classification based on Earth-based spectra: three compositional groups can be observed, and the trend of increasing mafic absorption band strength from Group 1 to Group 2 to Group 3 is noted. As redefined here, Group 1 deposits include those of Alphonsus West, Alphonsus Southeast, Alphonsus Northeast 2, Atlas South, Cru??ger, Franklin, Grimaldi, Lavoisier, Oppenheimer, Orientale, and Riccioli. Group 1 deposits resemble lunar highlands, with weak mafic bands and relatively high UV/VIS ratios. Group 2 deposits include those of Alphonsus Northeast 1, Atlas North, Eastern Frigoris East and West, and Aristarchus Plateau; Group 2 deposits are similar to mature lunar maria, with moderate mafic band depths and intermediate UV/VIS ratios. The single Group 3 deposit, J. Herschel, has a relatively strong mafic band and a low UV/VIS ratio, and olivine is a likely juvenile component. Two of the deposits in these groups, Orientale and Aristarchus, are large pyroclastic deposits. The third large pyroclastic deposit, Apollo 17/Taurus Littrow, has a very weak mafic band and a high UV/VIS ratio and it does not belong to any of the compositional groups for small pyroclastic deposits. The observed compositional variations indicate that highland and mare materials are also present in many large and small pyroclastic deposits, and they suggest that volcanic glasses or spheres may not be dominant juvenile components in all large pyroclastic deposits. Copyright 2000 by the American Geophysical Union. |
| Genre: | Article |
| ProdID: | 70022891 |
| Citation Author: | Gaddis, L. R.; Hawke, B. R.; Robinson, M. S.; Coombs, C. |
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| Citation End Page: | 4262 |
| Citation Issue: | E2 |
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| Citation Language: | English |
| Citation Larger Work Title: | Journal of Geophysical Research E: Planets |
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| Citation Number Of Pages: | 18 |
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| Citation Search Results Text: | Compositional analyses of small lunar pyroclastic deposits using Clementine multispectral data; 2000; Article; Journal; Journal of Geophysical Research E: Planets; Gaddis, L. R.; Hawke, B. R.; Robinson, M. S.; Coombs, C. |
| Citation Start Page: | 4245 |
| Citation Volume: | 105 |
| Citation Year: | 2000 |
| Type: | citation/reference |
| Text: | Compositional analyses of small lunar pyroclastic deposits using Clementine multispectral data; 2000; Article; Journal; Journal of Geophysical Research E: Planets; Gaddis, L. R.; Hawke, B. R.; Robinson, M. S.; Coombs, C. |
| URL (THUMBNAIL): | http://pubs.er.usgs.gov/thumbnails/outside_thumb.jpg |
| Date Other: | Sat, 1 Jan 2000 00:00 -0600 |
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