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The CM chondrites are characterized as primary accretionary rocks whichoriginate from primitive water-rich asteroids formed during the early SolarSystem. Here, we study the mineralogy and organic characteristics of right CMand one ungrouped chondrite to better understand their alteration history;Queen Alexandra Range 93005 (QUE 93005), Murchison, LaPaz Icefield 02333 (LAP02333), Miller Range (MIL 13005), Mackay Glacier 05231 (MCY 05231), NorthwestAfrica 8534 (NWA 8534), Northwest Africa 3340 (NWA 3340), Yamato 86695(Y-86695), and the ungrouped carbonaceous chondrite Belgica 7904 (B-7904).Raman spectroscopy has been employed to detect the presence of organic carbonin the samples, specifically through the G band at approximately 1580 cm-1 andD band at around 1350 cm-1. The properties of organic matter in meteoritesserve as valuable indicators for characterizing the structure and crystallinityof carbonaceous materials and estimating their thermal metamorphism degree. TheR1 parameter, defined as the peak height ratio of the D and G bands, provides aquantifiable measure of this structural organization. Raman spectra are used toshow the general mineralogy, thermal history and heating stage of CM andungrouped chondrites. X-ray diffraction patterns further indicate themineralogical compositions of the samples. Visible to near-infrared (VNIR) andattenuated total reflection (ATR) reflectance spectra illustrate the trendsrelated to their mineralogy and furthermore infer aqueous alteration, thermalhistory of CM carbonaceous chondrites, formation and evolution of their parentbodies.

Investigating Organic Carbon and Thermal History of CM Carbonaceous Chondrites Using Spectroscopy and Laboratory Techniques