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Title:
The granulitic impactite suite: Impact melts and metamorphic breccias of the early lunar crust
Authors:
Cushing, Janet A.; Taylor, G. Jeffrey; Norman, Marc D.; Keil, Klaus
Affiliation:
AA(Planetary Geosciences, Hawai'i Institute= of Geophysics and Planetology, 2525 Correa Rd., Honolulu, Hawai'i 96822,= USA; ), AB(Planetary Geosciences, Hawai'i Institute= of Geophysics and Planetology, 2525 Correa Rd., Honolulu, Hawai'i 96822,= USA; ), AC(Planetary Geosciences, Hawai'i Institute= of Geophysics and Planetology, 2525 Correa Rd., Honolulu, Hawai'i 96822,= USA; ), AD(Planetary Geosciences, Hawai'i Institute= of Geophysics and Planetology, 2525 Correa Rd., Honolulu, Hawai'i 96822,= USA; )
Publication:
Meteoritics & Planetary Science, vol. 34, no. 2, pp. 185-195 (1999).
Publication Date:
03/1999
Origin:
M&PS
Bibliographic Code:
1999M&PS...34..185C

Abstract

An important and poorly understood group of rocks found in the ancient lunar highlands is called "feldspathic granulitic impactites." Rocks of the granulite suite occur at most of the Apollo highlands sites as hand samples, rake samples, clasts in breccias, and soil fragments. Most lunar granulites contain 70-80% modal plagioclase, but they can range from anorthosite to troctolite and norite. Previous studies have led to different interpretations for the thermal history of these rocks, including formation as igneous plutons, long-duration metamorphism at high temperatures, and short-duration metamorphism at low temperatures. This paper reports on a study of 24 polished thin sections of lunar granulites from the Apollo 15, 16, and 17 missions. We identify three different textural types of granulitic breccias: poikilitic, granoblastic, and poikilitic-granoblastic breccias. These breccias have similar equilibration temperatures (1100 +/- 50 deg C), as well as common compositions. Crystal size distributions in two granoblastic breccias reveal that Ostwald ripening took place during metamorphism. Solid-state grain growth and diffusion calculations indicate relatively rapid cooling during metamorphism, 0.5 to 50 deg C/year, and thermal modeling shows that they cooled at relatively shallow depths (<200 m). In contrast, we conclude that the poikilitic rocks formed by impact melting, whereas the poikilitic-granoblastic rocks were metamorphosed and may have partially melted. These results indicate formation of lunar granulites in relatively small craters (30-90 km in diameter), physically associated with the impact-melt breccia pile, and possibly from fine-grained fragmental precursor lithologies.

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