The far side of the Moon

Introduction: The comprehensive study of composition, nature of crystalline structure, geologic setting, and diversity of primary anorthositic crust which were exposed at the lunar surface will reveal the better understanding of evolution history of the lunar crust [1,2]. The primary crust of anorthositic highlands of the Moon formed by the crystallization and flotation of plagioclase in the late stages of lunar magma ocean due to the density difference between plagioclase and the remaining mafic liquids [3,4,5]. The compositional variations in the lunar highlands indicate the two different broad group of rock units i.e., 1). The rocks are mostly anorthosites which termed as ferroan anorthosites that contain strong typical calcic plagioclase, 2). the magnesium rich rock units of noritic, troctolite, and dunite etc., The most of the impact craters and basins were filled by the mare deposits however the remnant of the primary crust materials (anorthositic) were still present at the those regions, which could help us to understand the contrast between mare and highland associated materials. The Moon Mineralogy Mapper (M) data was used to study the lunar anorthositic composition and its mixtures such as gabbroic, noritic, and troctolite anorthosites etc., to reveal the crustal diversity of highlands rocks [6,7]. In the present study, distribution of lunar anorthosites and their associated mixtures were studied in the mare emplaced Finsen and kovalevskaya craters on the far side of the moon.