Lunar sample 14425: Not a lunar tektite |
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| Affiliation: | 1. Department of Physics, Florida A&M University, 2077 E. Paul Dirac Drive, Tallahassee, FL 32310, United States;2. Alakai Defense Systems, 197 Replacement Ave, Suite 102, Fort Leonard Wood, MO 65473, United States;1. Department of Physics, Rikkyo University, 3-34-1 Nishi-Ikebukuro, Toshima, Tokyo 171-8501, Japan;2. Department of Complexity Science and Engineering, University of Tokyo, 5-1-5 Kashiwanoha, Kashiwa, Chiba 277-8561, Japan;3. Earthquake Research Institute, University of Tokyo, 1-1-1 Yayoi, Bunkyo, Tokyo 113-0032, Japan;4. Planetary Exploration Research Center, Chiba Institute of Technology, 2-17-1 Tsudanuma, Narashino, Chiba 275-0016, Japan;5. Hokkaido University Graduate School of Science, 8-2-10 Kita-10 Nishi-8, Kita-ku, Sapporo, Hokkaido 060-0810, Japan;6. Department of Earth and Environmental Sciences, Nagoya University, Furo Chikusa, Nagoya, Aichi 464-8601, Japan;7. National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan |
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| Abstract: | Energy-dispersive x-ray analysis of a polished section of lunar sample 14425 shows, in contradiction to a previous report, that it has a composition similar to Apollo 14 breccias, but not to high-magnesium microtektites. The glass is homogeneous, but the bead contains numerous metallic spherules up to 0.7 mm in diameter. The metal in the spherules is iron with up to 16 wt.% Ni and 9 wt.% P and small amounts of S and Si. The high phosphorus content indicates the presence of a fine-grained phosphide phase in the metal. All of the metallic spherules have an associated sulphide phase. The composition of the glass bead and the presence of numerous Ni-Fe spherules with an associated sulphide phase indicates that the bead was formed by impact melting of surficial deposits at the Apollo 14 site. |
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