Calcium-aluminum-rich inclusions and amoeboid olivine aggregates from the CR carbonaceous chondrites

Calcium-aluminum-rich refractory inclusions (CAIs) in CR chondrites are rare (<1 vol%), fairly small (<500 mum) and irregularly-shaped, and most of them are fragmented. Based on the mineralogy and petrography, they can be divided into grossite +/- hibonite-rich, melilite-rich, and pyroxene-anorthite-rich CAIs. Other types of refractory objects include fine-grained spinel-melilite-pyroxene aggregates and amoeboid olivine aggregates (AOAs). Some of the pyroxene-anorthite-rich CAIs have igneous textures, and most melilite-rich CAIs share similarities to both the fluffy and compact type A CAIs found in CV chondrites. One major difference between these CAIs and those in CV, CM, and CO chondrites is that secondary mineral phases are rare. In situ ion microprobe analyses of oxygen-isotopic compositions of 27 CAIs and AOAs from seven CR chondrites demonstrate that most of the CAIs are O-16-rich (Delta(17)O of hibonite, melilite, spinel, pyroxene, and anorthite < -22parts per thousand) and isotopically homogeneous within 3-4parts per thousand. Likewise, forsterite, spinel, anorthite, and pyroxene in AOAs have nearly identical, O-16-rich compositions (-24parts per thousand < Delta(17)O < -20parts per thousand). In contrast, objects which show petrographic evidence for extensive melting are not as O-16-rich (Delta(17)O less than -18parts per thousand). Secondary alteration minerals replacing O-16-rich melilite in melilite-rich CAIs plot along the terrestrial fractionation line. Most CR CAIs and AOAs are mineralogically pristine objects that largely escaped thermal metamorphism and secondary alteration processes, which is reflected in their relatively homogeneous O-16-rich compositions. It is likely that these objects (or their precursors) condensed in an O-16-rich gaseous reservoir in the solar nebula. In contrast, several igneous CAIs are not very enriched in O-16, probably as a result of their having melted in the presence of a relatively O-16-poor nebular gas. If the precursors of these CAIs were as O-16-rich as other CR CAIs, this implies either temporal excursions in the isotopic composition of the gas in the CAI-forming regions and/or radial transport of some CAI precursors into an O-16-poor gas. The absence of oxygen isotope heterogeneity in the primary minerals of melilite-rich CAIs containing alteration products suggests that mineralogical alteration in CR chondrites did not affect oxygen-isotopic compositions of their CAIs.