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• W1661008983 abstract "Introduction: Lunar mare basalts are products of partial melting of the lunar mantle, serving as probes of the composition, structure, and thermal history of the inaccessible lunar interior. Cryptomaria are covered mare deposits that are obscured from view by the subsequent emplacement of ejecta from craters and basins. They are keys to understand ancient mare volcanism, predating the younger volcanism represented by exposed maria sampled by Apollo and Luna missions. Studies by ground-based observations and lunar orbital satellites have revealed that the cryptomaria are widely distributed on the surface of the Moon [e.g. 1]. Yet, their nature is not well defined, due to the lack of the ground truth. Here, we report a group of Antarctic lunar meteorites of cryptomaria origin with reasonable certainty. Samples description: Four Antarctic lunar meteorites, Yamato (Y) 793169, Asuka (A) 881757, Meteorite Hills (MET) 01210, and Miller Range (MIL) 05035 (YAMM meteorites) are paired low-Ti (∼2 wt% TiO2) mare basalts [2]. MET 01210 is a regolith breccia with mixture of mare and highland components, including a basalt clast 2.7× 4.7 mm in size. The other three are unbrecciated basalt (Fig. 1). They are probably derived from a single basalt flow of >100 m thick [2] extruded at 3870 Ma [e.g. 3], and were simultaneously launched off the Moon at 1 Ma [e.g. 4]. Methods: On the basis of mineralogical data of the above four meteorites [2] combined with the bulk chemistry data, cosmic exposure record, and isotopic age from other studies, a possible source crater of the meteorites was identified, utilizing global maps of FeO, TiO2, optical maturity (OMAT) image from Clementine UV-VIS camera and Th data from Lunar Prospector gamma-ray spectrometer. Results and discussions: The low surface irradiation and low maturity of MET 01210, which are similar to those of Apollo 16 regolith breccias, represent ancient regolith residing beneath the surface regolith [5]. As the surface regolith thickness is generally a few meters in mare areas [6], the burial depth of > several meters for the YAMM meteorites clearly indicate that they are originated from regions enriched in mare materials, other than the exposed mare areas. The extremely short exposure time for 3870 Ma-aged YAMM meteorites is in line with the higher turnover rates due to intense meteoroid bombardment, ∼3900 Ma [5]. With these grounds, the YAMM meteorites reasonably represent an ancient mare basalt flow, which has little chance to be exposed on the surface, that is, cryptomaria. While source craters of brecciated lunar meteorites are generally a few km in diameter, those of crystalline ones which are mechanically stronger than breccias tend to be smaller and less than 1 km (i.e. 0.9 km source crater for A-881757) [7]. The size of the source crater which simultaneously ejected crystalline basalts and brecciated basalts would be smaller than a few km." @default.
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• W1661008983 date "2008-03-01" @default.
• W1661008983 modified "2023-09-28" @default.
• W1661008983 title "Antarctic Lunar Meteorites from Cryptomaria of the Moon" @default.
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