The presolar grain inventory of fine‐grained chondrule rims in the Mighei‐type (CM) chondrites. (21st November 2019)

• Record Type: Journal Article
• Authors: Leitner, Jan; Metzler, Knut; Vollmer, Christian; Floss, Christine; Haenecour, Pierre; Kodolányi, János; Harries, Dennis; Hoppe, Peter
• Is Part Of: Meteoritics & planetary science. Volume 55:Number 6(2020)
• Page Start: 1176
• Page End: 1206
• Publication Date: 2019-11-21
• Subjects: Meteorites -- Periodicals; Planetology -- Periodicals; 523.4
• DOI: 10.1111/maps.13412
• Languages: English
• ISSNs: 1086-9379

Abstract

Abstract: We investigated the inventory of presolar silicate, oxide, and silicon carbide (SiC) grains of fine‐grained chondrule rims in six Mighei‐type (CM) carbonaceous chondrites (Banten, Jbilet Winselwan, Maribo, Murchison, Murray and Yamato 791198), and the CM‐related carbonaceous chondrite Sutter's Mill. Sixteen O‐anomalous grains (nine silicates, six oxides) were detected, corresponding to a combined matrix‐normalized abundance of ~18 ppm, together with 21 presolar SiC grains (~42 ppm). Twelve of the O‐rich grains are enriched in 17 O, and could originate from low‐mass asymptotic giant branch stars. One grain is enriched in 17 O and significantly depleted in 18 O, indicative of additional cool bottom processing or hot bottom burning in its stellar parent, and three grains are of likely core‐collapse supernova origin showing enhanced 18 O/ 16 O ratios relative to the solar system ratio. We find a presolar silicate/oxide ratio of 1.5, significantly lower than the ratios typically observed for chondritic meteorites. This may indicate a higher degree of aqueous alteration in the studied meteorites, or hint at a heterogeneous distribution of presolar silicates and oxides in the solar nebula. Nevertheless, the low O‐anomalous grain abundance is consistent with aqueous alteration occurring in the protosolar nebula and/or on the respective parent bodies. Six O‐rich presolar grains were studied by Auger Electron Spectroscopy, revealing two Fe‐rich silicates, one forsterite‐like Mg‐rich silicate, two Al‐oxides with spinel‐like compositions, and one Fe‐(Mg‐)oxide. Scanning electron and transmission electron microscopic investigation of a relatively large silicate grain (490 nm × 735 nm) revealed that it was crystalline åkermanite (Ca2 Mg[Si2 O7 ]) or a an åkermanite‐diopside (MgCaSi2 O6 ) intergrowth.