[P-PS06] 月の科学と探査

[PPS06-P11] 月表面のカンラン石と斜長石に富む岩石の共存サイトに対する将来のサンプルリターンミッションの候補地としての可能性の検討

*山本 聡¹、唐牛 譲、長岡 央⁴、石原 吉明²、大竹 真紀子³、鹿山 雅裕⁵ (1.国立研究開発法人 産業技術総合研究所、2.JAXA 国際宇宙探査センター、3.会津大学、4.理化学研究所、5.東京大学)

キーワード：リモートセンシング、かぐや/SELENE、月鉱物

So far, 14 sites of co-existing occurrences (co-existing sites) of olivine- and plagioclase-rich rocks have been identified located around large impact basins, including the Moscoviense, Crisium, Imbrium, and Schrödinger basins [1]. At these sites, purest anorthosite (PAN) rocks [2,3], which consist of more than 98% plagioclase, occur adjacent to olivine-rich rocks. The PAN rocks are thought to be remnants of the primitive crust formed during the cooling process of magma oceans in the early stages of lunar formation, and the olivine-rich rocks could have been excavated from the lunar mantle during the formation of impact basins. Thus, understanding how co-existing sites of olivine- and plagioclase-rich rocks are formed will lead to a better understanding of the structure, composition, and evolution of the lunar mantle and crust. Therefore, for future sample return missions, it is expected that the co-existing sites of olivine- and plagioclase-rich rocks would be a “one-stop” site that provides important information for the overall characterization of lunar mantle and crustal materials. According to [1], the geology of the co-existing occurrences can be divided into three geological types: (1) co-existing occurrences associated with impact craters, (2) cliffs or steep slopes of the peak rings and rims of impact basins, and (3) the central peaks of the large complex craters. However, it is also important to consider the accessibility of each geological type as potential sites for future sample returns and in-situ measurements. In this presentation, we will discuss the accessibility of these coexisting sites based on the results of stratigraphic analysis using the Multiband Imager data and the Digital Elevation Model from the Terrain Camera onboard Kaguya/SELENE.



[1] Yamamoto et al. (2022), Journal of Geophysical Research: Planets, 127, e2021JE007077, doi 10.1029/2021JE007077

[2] Ohtake et al. (2009), Nature, 461, 236, doi: 10.1038/nature08317

[3] Yamamoto et al. (2012) Geophysical Research Letters, 39, doi: 0.1029/2012GL052098.