Geochemical Characterization of Lunar Meteorites via Raman Spectroscopy: Implications for Planetary Differentiation and Comparative Analysis

Lunar meteorites are a key source of information for understanding the Moon’s geochemical structure and evolutionary history. Unlike Apollo samples, they originate from diverse and often unsampled regions, offering broader insights into volcanic activity, impact events, and differentiation processes. Each meteorite type provides a unique glimpse into different lunar periods, contributing to a more comprehensive understanding of the Moon’s evolution.

A crucial aspect of their study is the detailed investigation of mineral phases. Key questions include the growth history of minerals, chemical zoning, fluid inclusions, and overprinting by melts or impacts. Raman spectroscopy is employed for initial, non-destructive mineral identification. This is followed by electron microprobe analysis and scanning electron microscopy (SEM) for high-resolution compositional data.

The Mineralogical State Collection Munich (MSM) operates a dedicated Raman laboratory and maintains the MSM-MRD database, a growing reference for laboratory and in-situ spectroscopy. Lunar meteorites significantly contribute to this database, enhancing Raman spectral libraries essential for future space missions using remote sensing and in-situ analysis.

Beyond lunar samples, our research includes meteorites from Mars, Vesta, pallasites, and chondrites. These are compared with terrestrial analogs—such as mantle xenoliths and ophiolitic rocks—to better understand planetary differentiation and magmatic evolution. Lunar meteorites, in particular, offer a more representative view of the Moon’s surface and chemistry than Apollo samples alone.

This work supports the advancement of planetary spectroscopy, contributing to the interpretation of spectroscopic data and preparing the ground for future robotic and human exploration missions.