|Title:||Oxygen‐isotopic compositions of low‐FeO relicts in high‐FeO host chondrules in Acfer 094, a type‐3.0 carbonaceous chondrite closely related to CM|
|Authors:||T. Kunihiro, A.E. Rubin, and J.T. Wasson|
|Publication:||Geochim. Cosmochim. Acta., v. 69, p. 3831‐3840.|
|Publish Date:||Aug 2005|
With one exception, the low‐FeO relict olivine grains within high‐FeO porphyritic chondrules in the type 3.0 Acfer 094 carbonaceous chondrite have Δ17O (=δ17O − 0.52 × δ18O) values that are substantially more negative than those of the high‐FeO olivine host materials. These results are similar to observations made earlier on chondrules in CO3.0 chondrites and are consistent with two independent models: (1) Nebular solids evolved from low‐FeO, low‐Δ17O compositions towards high−FeO, more positive Δ17O compositions; and (2) the range of compositions resulted from the mixing of two independently formed components. The two models predict different trajectories on a Δ17O vs. log Fe/Mg (olivine) diagram, but our sample set has too few values at intermediate Fe/Mg ratios to yield a definitive answer. Published data showing that Acfer 094 has higher volatile contents than CO chondrites suggest a closer link to CM chondrites. This is consistent with the high modal matrix abundance in Acfer 094 (49 vol.%). Acfer 094 may be an unaltered CM chondrite or an exceptionally matrix‐rich CO chondrite. Chondrules in Acfer 094 and in CO and CM carbonaceous chondrites appear to sample the same population. Textural differences between Acfer 094 and CM chondrites are largely attributable to the high degree of hydrothermal alteration that the CM chondrites experienced in an asteroidal setting.