[PPS10-10] Evidence for an 16O-poor gaseous reservoir during formation of a fine-grained CAI from Northwest Africa 8613
The FGI HKD01 has an irregular shape with a size of approximately 10 × 12 mm and composed mainly of melilite, hibonite, and spinel. O-isotope compositions of the constituent minerals plot along the CCAM line, ranging between Δ17O ~ −23‰ and 0‰. The FGI is petrographically four layered structure from core to rim as hibonite-rich core, spinel-rich core, melilite-rich mantle, and hibonite-spinel-melilite-rich mantle. Each petrographic domain contains melilite, hibonite, and spinel with variable proportions of those minerals. The FGI is rimmed by thin spinel and diopside layers. The spinel and hibonite grains in the FGI are uniformly 16O-rich (Δ17O = −23‰). Melilite crystals in the two cores exhibit normal chemical zoning with O-isotope zoning from Δ17O ~ −23‰ to −14‰. Melilite crystals in the hibonite-spinel-melilite-rich mantle exhibit normal chemical zoning with O-isotope zoning from Δ17O ~ −17‰ to 0‰. Melilite crystals in the melilite-rich mantle show chemical oscillatory zoning with uniform 16O-poor (Δ17O ~ 0‰) value despite their chemical variations (Åk2−14). Crystal sizes of melilite in the core and the hibonite-spinel-melilite-rich mantle are generally less than 10 µm, while those of melilite in the melilite-rich mantle are typically 15 to 25 µm.
Therefore, in the FGI, intra-crystalline distribution of O-isotopes is homogeneous in larger melilite, but heterogeneous in smaller melilite. This contrast for O-isotope distribution indicates that the O isotopic compositions in melilite of the FGI HKD01 have not been disturbed significantly by secondary processes because the exchange rate is dependent on crystal sizes [6, 7]. The O-isotope distribution of melilite in the FGI HKD01 correspond to those of nebular gas at the FGI condensed. Our data imply that both 16O-rich and 16O-poor gaseous reservoirs co-existed in the forming region of the FGI HKD01. The Al−Mg systematics of the FG-CAI indicate that these formation events occurred at 0.09 ± 0.02 Myr after the formation of canonical CAIs , if 26Al was homogeneously distributed.
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