Water in evolved lunar rocks: Evidence for multiple reservoirs

1,2,3Katharine L. Robinson, 4,5Jessica J. Barnes, 1Kazuhide Nagashima, 1Aurélien Thomen, 5Ian A. Franchi, 1,2,3Gary R. Huss, 4,5Mahesh Anand, 1,2,3G. Jeffrey Taylor
1Hawaii Institute of Geophysics and Planetology, 1680 East-West Rd. POST 602, Honolulu, HI 96822, USA
2University of Hawaii NASA Astrobiology Institute, Institute for Astronomy, University of Hawai’i, 2680 Woodlawn Drive, Honolulu, Hawaii 96822-1839, USA
3Geology and Geophysics, University of Hawaii at Manoa, 1680 East-West Rd. POST 602, Honolulu, HI 96822, USA
4Planetary and Space Sciences, The Open University, Walton Hall, Milton Keynes, MK7 6AA, UK
5Department of Earth Sciences, The Natural History Museum, Cromwell Road, London, SW7 5BD, UK

We have measured the abundance and isotopic composition of water in apatites from several lunar rocks representing Potassium (K), Rare Earth Elements (REE), and Phosphorus (P) – KREEP – rich lithologies, including felsites, quartz monzodiorites (QMDs), a troctolite, and alkali anorthosite. The H-isotope data from apatite provide evidence for multiple reservoirs in the lunar interior. Apatite measurements from some KREEP-rich intrusive rocks display moderately elevated δD signatures, while other samples show δD signatures similar to the range known for the terrestrial upper mantle. Apatite grains in Apollo 15 quartz monzodiorites have the lowest δD values measured from the Moon so far (as low as – 749 ‰), and could potentially represent a D-depleted reservoir in the lunar interior that had not been identified until now. Apatite in all of these intrusive rocks contains < 267 ppm H2O, which is relatively low compared to apatites from the majority of studied mare basalts (200 to > 6500 ppm H2O). Complexities in partitioning of volatiles into apatite make this comparison uncertain, but measurements of residual glass in KREEP basalt fragments in breccia 15358 independently show that the KREEP basaltic magmas were low in water. The source of 15358 contained ∼ 10 ppm H2O, about an order of magnitude lower than the source of the Apollo 17 pyroclastic glass beads, suggesting potential variations in the distribution of water in the lunar interior.

Reference
Robinson KL, Barnes JJ, Nagashima K, Thomen A, Franchi IA, Huss GR, Anand M, Taylor GJ (2016) Water in evolved lunar rocks: Evidence for multiple reservoirs. Geochimica et Cosmochmica Acta (in Press)
Link to Article [doi:10.1016/j.gca.2016.05.030]
Copyright Elsevier

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