The origin of young mare basalts inferred from lunar meteorites Northwest Africa 4734, 032, and LaPaz Icefield 02205 |
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| Authors: | Stephen M Elardo Charles K Shearer Jr Amy L Fagan Lars E Borg Amy M Gaffney Paul V Burger Clive R Neal Vera A Fernandes Francis M McCubbin |
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| Institution: | 1. Department of Earth & Planetary Sciences, Institute of Meteoritics, University of New Mexico, , Albuquerque, New Mexico, 87131 USA;2. Department of Civil & Environmental Engineering & Earth Sciences, University of Notre Dame, , Notre Dame, Indiana, 46556 USA;3. Lunar & Planetary Institute, USRA, , Houston, Texas, 77058 USA;4. Chemical Sciences Division, Lawrence Livermore National Laboratory, , Livermore, California, 94550 USA;5. Museum für Naturkunde‐ Berlin, Leibniz‐Institut für Evolutions‐ und Biodiversit?tsforschung, , 10115 Berlin, Germany |
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| Abstract: | Northwest Africa (NWA) 4734 is an unbrecciated basaltic lunar meteorite that is nearly identical in chemical composition to basaltic lunar meteorites NWA 032 and LaPaz Icefield (LAP) 02205. We have conducted a geochemical, petrologic, mineralogic, and Sm‐Nd, Rb‐Sr, and Ar‐Ar isotopic study of these meteorites to constrain their petrologic relationships and the origin of young mare basalts. NWA 4734 is a low‐Ti mare basalt with a low Mg* (36.5) and elevated abundances of incompatible trace elements (e.g., 2.00 ppm Th). The Sm‐Nd isotope system dates NWA 4734 with an isochron age of 3024 ± 27 Ma, an initial εNd of +0.88 ± 0.20, and a source region 147Sm/144Nd of 0.201 ± 0.001. The crystallization age of NWA 4734 is concordant with those of LAP 02205 and NWA 032. NWA 4734 and LAP 02205 have very similar bulk compositions, mineral compositions, textures, and ages. Their source region 147Sm/144Nd values indicate that they are derived from similar, but distinct, source materials. They probably do not sample the same lava flow, but rather are similarly sourced, but isotopically distinct, lavas that probably originate from the same volcanic complex. They may have experienced slightly different assimilation histories in route to eruption, but can be source‐crater paired. NWA 032 remains enigmatic, as its source region 147Sm/144Nd definitively precludes a simple relationship with NWA 4734 and LAP 02205, despite a similar bulk composition. Their high Ti/Sm, low (La/Yb)N, and Cl‐poor apatite compositions rule out the direct involvement of KREEP. Rather, they are consistent with low‐degree partial melting of late‐formed LMO cumulates, and indicate that the geochemical characteristics attributed to urKREEP are not unique to that reservoir. These and other basaltic meteorites indicate that the youngest mare basalts originate from multiple sources, and suggest that KREEP is not a prerequisite for the most recent known melting in the Moon. |
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