Origin of Low-26Al/27Al Corundum/Hibonite Inclusions in Meteorites

Most meteoritic calcium-rich, aluminum-rich inclusions formed from a reservoir with Al-26/Al-27 approximate to 5 x 10(-5), but some record lower (Al-26 Al-27)0, demanding they sampled a reservoir without live Al-26. This has been interpreted as evidence for "late injection" of supernova material into our protoplanetary disk. We instead interpret the heterogeneity as chemical, demonstrating that these inclusions are strongly associated with the refractory phases corundum or hibonite. We name them "low-Al-26/Al-27 corundum/hibonite inclusions" (LAACHIs). We present a detailed astrophysical model for LAACHI formation in which they derive their Al from presolar corundum, spinel, or hibonite grains 0.5-2 mu m in size with no live Al-26; live Al-26 is carried on smaller (<50 nm) presolar chromium spinel grains from recent nearby Wolf-Rayet stars or supernovae. In hot (approximate to 1350-1425 K) regions of the disk, these grains and perovskite grains would be the only survivors. These negatively charged grains would grow to sizes 1-10(3) mu m, even incorporating positively charged perovskite grains, but not the small, negatively charged Al-26-bearing grains. Chemical and isotopic fractionations due to grain charging was a significant process in hot regions of the disk. Our model explains the sizes, compositions, oxygen isotopic signatures, and the large, correlated Ca-48 and Ti-50 anomalies (if carried by presolar perovskite) of LAACHIs, and especially how they incorporated no Al-26 in a solar nebula with uniform, canonical Al-26/Al-27. A late injection of supernova material is obviated, although formation of the Sun in a high-mass star-forming region is demanded.