Coarse-grained igneous Ca,Al-rich inclusions (CAIs) in CV (Vigarano group) carbonaceous chondrites have typically heterogeneous O-isotope compositions with melilite, anorthite, and high-Ti (>10 wt% TiO2) fassaite being O-16-depleted (Delta O-17 up to similar to - 3 +/- 2 parts per thousand) compared to hibonite, spinel, low-Ti (<10 wt% TiO2) fassaite, Al-diopside, and forsterite, all having close-to-solar Delta O-17 similar to - 24 +/- 2 parts per thousand. To test a hypothesis that this heterogeneity was established, at least partly, during aqueous fluid-rock interaction, we studied the mineralogy, petrology, and O-isotope compositions of igneous CAIs CG-11 (Type B), TS-2F-1, TS-68, and 818-G (Compact Type A), and 818-G-UR (davisite-rich) from Allende (CV > 3.6), and E38 (Type B) from Efremovka (CV3.1-3.4). Some of these CAIs contain (i) eutectic mineral assemblages of melilite, Al,Ti-diopside, and +/- spinel which co-crystallized and therefore must have recorded O-isotope composition of the eutectic melt; (ii) isolated inclusions of Ti-rich fassaite inside spinel grains which could have preserved their initial O-isotope compositions, and/or (iii) pyroxenes of variable chemical compositions which could have recorded gas-melt O-isotope exchange during melt crystallization and/or postcrystallization exchange controlled by O-isotope diffusivity. If these CAIs experienced isotopic exchange with an aqueous fluid, O-isotope compositions of some of their primary minerals are expected to approach that of the fluid. We find that in the eutectic melt regions composed of highly-akermanitic melilite (angstrom k(65-71)), anorthite, low-Ti fassaite, and spinel of E38, spinel, fassaite, and anorthite are similarly O-16-rich (Delta O-17 similar to- 24 parts per thousand), whereas melilite is O-16-poor (Delta O-17 similar to- 1 parts per thousand). In the eutectic melt regions of CG-11, spinel and low-Ti fassaite are O-16-rich (Delta O-17 similar to- 24 parts per thousand), whereas melilite and anorthite are O-16-poor (Delta O-17 similar to- 3 parts per thousand). In TS-2F-1, TS-68, and 818-G, melilite and high-Ti fassaite grains outside spinel have O-16-poor compositions (Delta O-17 range from - 12 to - 3 parts per thousand); spinel is O-16-rich (Delta O-17 similar to- 24 parts per thousand); perovskite grains show large variations in Delta O-17, from - 24 to - 1 parts per thousand. Some coarse perovskites are isotopically zoned with a O-16-rich core and a O-16-poor edge. Isolated high-Ti fassaite inclusions inside spinel grains are O-16-rich (Delta O-17 similar to- 24 parts per thousand), whereas high-Ti fassaite inclusions inside fractured spinel grains are O-16-depleted: Delta O-17 range from - 12 to - 3 parts per thousand. In 818-G-UR, davisite is O-16-poor (Delta O-17 similar to- 2 parts per thousand), whereas Al-diopside of the Wark-Lovering rim is O-16-enriched (Delta O-17 similar to- 16 parts per thousand). On a three-isotope oxygen diagram, the O-16-poor melilite, anorthite, high-Ti fassaite, and davisite in the Allende CAIs studied plot close to O-isotope composition of an aqueous fluid (Delta O-17 similar to- 3 +/- 2 parts per thousand) inferred from O-isotope compositions of secondary minerals resulted from metasomatic alteration of the Allende CAIs. We conclude that CV igneous CAIs experienced post-crystallization O-isotope exchange that most likely resulted from an aqueous fluid-rock interaction on the CV asteroid. It affected melilite, anorthite, high-Ti fassaite, perovskite, and davisite, whereas hibonite, spinel, low-Ti fassaite, Al-diopside, and forsterite retained their original O-isotope compositions established during igneous crystallization of CV CAIs. However, we cannot exclude some gas-melt O-isotope exchange occurred in the solar nebula. This apparently "mineralogically-controlled" exchange process was possibly controlled by variations in oxygen self-diffusivity of CAI minerals. Experimentally measured oxygen self-diffusion coefficients in CAI-like minerals are required to constrain relative roles of O-isotope exchange during aqueous fluid-solid and nebular gas-melt interaction. (C) 2022 Elsevier Ltd. All rights reserved.
