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Project Progress

We have analyzed OH concentrations in the mineral apatite, using our Cameca 1280 SIMS. The distinguishing feature of our work is that we have concentrated on rocks that are rich in trace elements that do not readily enter into major minerals as magma crystallizes, such as the rare earth elements. Specifically, we have been working on samples that are associated with KREEP basalt magmas. H₂O should also be highly enriched in these samples, according to well established understanding of how the lunar magma ocean (the primary lunar differentiation event) crystallized. Equally important, we have focused our attention on samples whose mineralogy and rock textures indicate crystallization in magma bodies that intruded at depth in the lunar crust. The higher pressure associated with these samples allows water to remain dissolved in the magma, preventing loss and D/H fractionation. We also measured the H content in a glassy KREEP basalt. The results show unambiguously that KREEP has much less water (possibly a factor of 100 less) than mare basalt and glassy mare deposit formed by fire fountains on the ancient Moon. In addition, D/H is distinctly higher in lunar water than in the Earth. While we cannot yet rule out that the initial lunar D/H was similar to that of the Earth (some processes do fractionate the two isotopes), it seems likely that lunar water has higher D/H than does terrestrial water. It is also possible that the water in KREEP is primary – accreted to the Moon when it formed – while the water in mare basalts and pyroclastic deposits was added after the magma ocean had crystallized. Deciding between alternative sources of water will require additional analyses and modeling to understand D/H fractionation in the proto-lunar disk and in magmas generated inside the Moon. Disk processes are being studied in collaboration with Steve Desch at Arizona State University.