¹Yuchen Xu,²Yangting Lin,²Jialong Hao,²Sen Hu,²Wei Yang,¹Yongliao Zou,¹Yang Liu
Meteoritics & Planetary Science (in Press) Link to Article [https://doi.org/10.1111/maps.14380]
¹State Key Laboratory of Solar Activity and Space Weather, National Space Science Center, Chinese Academy of Sciences, Beijing, China
²Key Laboratory of Earth and Planetary Physics, Institute of Geology and Geophysics, Chinese Academy of Sciences, Beijing, China
Published by arrangement with John Wiley & Sons

NWA 10493 and NWA 10498, two hot desert finds, are classified as the CO3.0 meteorites based on the Cr2O3 contents in ferroan olivines, representing some of the most primitive chondrites from the CO parent body. The abundances of presolar grains are known to be sensitive to the degree of aqueous alteration and thermal metamorphism. Therefore, an in situ investigation of presolar grains was conducted in the fine-grained matrix of NWA 10493 and NWA 10498 using NanoSIMS C- and O-isotopic image mapping. The matrix-normalized abundance of presolar SiC grains in NWA 10493 is
ppm, which declines to
ppm when the much larger (>1000 nm) grain is excluded. This lower presolar SiC abundance is comparable to the presolar SiC abundance of
ppm calculated in NWA 10498, similar to those from the most aqueously altered CM chondrites based on in situ studies of the fine-grained rims of chondrules. The abundances of O-anomalous grains in both NWA 10493 (54 ± 15 ppm) and NWA 10498 (42 ± 13 ppm) are lower than those reported for the most primitive CO meteorites, indicating slightly higher degrees of thermal alterations. These findings are consistent with the previously observed variations in Cr content within the respective chondrule olivine and point toward classification grades of 3.02–3.05.