1C.D. Williams, 2T. Ushikubo, 3E.S. Bullock, 1P.E. Janney, 1R.R. Hines, 2N.T. Kita,
1R.L. Hervig, 3G.J. MacPherson, 4R.A. Mendybaev,4F.M. Richter,1M. Wadhwa
Geochimica et Cosmochimica Acta (in Press) Link to Article [http://dx.doi.org/10.1016/j.gca.2016.10.053]
1School of Earth and Space Exploration, Arizona State University, Tempe, AZ 85287, United States
2WiscSIMS, Department of Geosciences, University of Wisconsin, Madison, WI 53706, United States
3Department of Mineral Sciences, National Museum of Natural History, Smithsonian Institution, Washington, DC 20560, United States
4Department of Geophysical Sciences, University of Chicago, Chicago, IL 60637, United States
Detailed petrologic, geochemical and isotopic analyses of a new FUN CAI from the Allende CV3 meteorite (designated CMS-1) indicate that it formed by extensive melting and evaporation of primitive precursor material(s). The precursor material(s) condensed in a 16O-rich region (δ17O and δ18O ∼ -49‰) of the inner solar nebula dominated by gas of solar composition at total pressures of ∼10-3 to 10-6 bar. Subsequent melting of the precursor material(s) was accompanied by evaporative loss of magnesium, silicon and oxygen resulting in large mass-dependent isotope fractionations in these elements (δ25Mg = 30.71 – 39.26‰, δ29Si = 14.98 – 16.65‰, and δ18O = -41.57 – -15.50‰). This evaporative loss resulted in a bulk composition similar to that of compact Type A and Type B CAIs, but very distinct from the composition of the original precursor condensate(s). Kinetic fractionation factors and the measured mass-dependent fractionation of silicon and magnesium in CMS-1 suggest that ∼ 80% of the silicon and ∼85% of the magnesium were lost from its precursor material(s) through evaporative processes. These results suggest that the precursor material(s) of normal and FUN CAIs condensed in similar environments, but subsequently evolved under vastly different conditions such as total gas pressure. The chemical and isotopic differences between normal and FUN CAIs could be explained by sorting of early solar system materials into distinct physical and chemical regimes, in conjunction with discrete heating events, within the protoplanetary disk.