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Using AOIs to Document Aqueous Alteration in the CO 3 Astroidal Parent Bodies

Introduction Chondritic meteorites are some of the solar system’s earliest aggregates. It is thought that chondritic meteorites come from small (<500km) asteroids because they were never molten (FeNi metal is still dispersed throughout the meteorites) and there is a similarity in the reflectance spectra between the chondrites and C-type asteroids. Radioactive dating with long-lived nuclides (e.g. Pb, Pb, U, Sm-Nd, and Rb-Sr) of Ca-Al-rich inclusions (CAIs) within chondritic meteorites show they must have formed 4.55 Ga ago. This dating indicates that chondritic meteorites show CAIs must have formed just after the Sun and before the planets accreted. Furthermore, chondritic meteorites are thought to have formed in this solar system because their bulk compositions are nearly identical to that of the solar photosphere, indicating that they are probably very primitive representatives of the early solids to have formed in the solar nebula. Chondritic meteorites have experienced few changes, compositional or otherwise, since formation and are studied to understand how these first solids formed. The subtle changes that are seen are from aqueous and thermal sources and must have occurred early in the formation of the solar system. Short-lived radio-nuclides (e.g. Mn) indicate that the formation of carbonate assemblages occurred within 10 Ma of CAI formation. Studying these alteration effects can give clues about the role of water and heat in the early solar system.