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Abundant presolar silicates of the CM chondrite Asuka 12169: Implications for the thermal and aqueous alteration of the CM parent body

文献类型：期刊论文

作者Xu, Yuchen3; Lin, Yangting2; Hao, Jialong2; Kimura, Makoto1; Hu, Sen2; Yang, Wei2; Liu, Yang3; Zou, Yongliao3
刊名GEOCHIMICA ET COSMOCHIMICA ACTA
出版日期2022-10-01
卷号334页码:45-64
ISSN号0016-7037
关键词CM Carbonaceous chondrites Asteroids Aqueous alteration Presolar grains NanoSIMS
DOI10.1016/j.gca.2022.07.016
英文摘要The solar system could be separated into two zones based on the isotopic dichotomy between non-carbonaceous and carbonaceous groups, with the latter likely accreted in the outer solar system. Among carbonaceous groups, the CM chondrite contains high abundances of organic carbon and water. They have undergone aqueous alteration, thermal metamorphism and brecciation to different degrees (e.g., Rubin et al., 2007; Tonui et al., 2014; Zolensky et al., 1997), which contributed to erasing most of the solar nebular records. Asuka 12169 was reported as the most primitive CM chondrite based on petrological and geochemical results, with little aqueous alteration (Kimura et al., 2020). In this paper, we report a survey of presolar grains in the fine-grained matrix and the accretionary rims of chondrules and CAIs in this meteorite, based on NanoSIMS mapping of C-, O-, and Si-isotopes. A total of 158 presolar grains were identified, including 119 silicates/oxides (208 +/- 20 ppm), 38 SiC (73 +/- 12 ppm) and 1 carbonaceous grain (2 + 5(-2) ppm). These abundances are within the maximum abundance ranges of prim-itive chondrites (80-280 ppm for O-rich grains and 10-180 ppm for C-rich grains). In comparison with most CM chondrites (< 40 ppm), Asuka 12169 is uniquely rich in presolar silicates (185 +/- 18 ppm), with a high presolar silicate/oxide ratio of-8, therefore providing robust evidence for little aqueous alteration. The high abundances of presolar SiC and silicates in Asuka 12169 clearly show its pristine properties regarding both thermal and aqueous alteration. Group 1, 2, 3 and 4 subtypes of presolar O-rich grains account for 84%, 2.5%, 0.8% and 12.6%, respectively. One O-rich grain shows a high enhancement in O-17/O-16 and a subsolar O-18/O-16 ratio (O-17/O-16 = 6.45 +/- 0.09 x 10(-3) and O-18/O-16 = 1.90 +/- 0.02 x 10-3), indicating a stellar origin in binary star systems or novae. Most identified presolar SiC are mainstream grains of AGB origins. One with 28Si-excess is classified as an X grain, suggesting a supernova origin. There are two SiC grains that have C-12/C-13 < 10 but close-to-solar Si isotopic ratios, and are therefore classified as AB type. The pristine features of Asuka 12169 suggest that it was probably located in the outermost few kilometers of the CM asteroid, where temperature was high enough for sublimation of water ice under vacuum, but where no aqueous alteration occurred, and where the depth was enough for lithifica-tion. The high abundances of various types of presolar grains, together with the petrographic information of Asuka 12169, provide crucial constrains on the original properties and subsequent evolution of the CM asteroids. (c) 2022 Elsevier Ltd. All rights reserved.
WOS关键词SILICON-CARBIDE GRAINS ; TITANIUM ISOTOPIC COMPOSITIONS ; RED GIANT STARS ; CARBONACEOUS CHONDRITE ; OXYGEN-ISOTOPE ; PRIMITIVE CHONDRITES ; SIC GRAINS ; MURCHISON ; METEORITE ; ORIGIN
资助项目Natural Science Foundation of China[41973064] ; Natural Science Foundation of China[41673069] ; Strategic Priority Research Program on Space Science, Chinese Academy of Sciences[XDA15020300] ; Strategic Priority Research Program on Space Science, Chinese Academy of Sciences[XDB41000000] ; JSPS KAKENHI[18K03729]
WOS研究方向Geochemistry & Geophysics
语种英语
出版者PERGAMON-ELSEVIER SCIENCE LTD
WOS记录号WOS:000840891600001
资助机构Natural Science Foundation of China ; Natural Science Foundation of China ; Natural Science Foundation of China ; Natural Science Foundation of China ; Strategic Priority Research Program on Space Science, Chinese Academy of Sciences ; Strategic Priority Research Program on Space Science, Chinese Academy of Sciences ; Strategic Priority Research Program on Space Science, Chinese Academy of Sciences ; Strategic Priority Research Program on Space Science, Chinese Academy of Sciences ; JSPS KAKENHI ; JSPS KAKENHI ; JSPS KAKENHI ; JSPS KAKENHI ; Natural Science Foundation of China ; Natural Science Foundation of China ; Natural Science Foundation of China ; Natural Science Foundation of China ; Strategic Priority Research Program on Space Science, Chinese Academy of Sciences ; Strategic Priority Research Program on Space Science, Chinese Academy of Sciences ; Strategic Priority Research Program on Space Science, Chinese Academy of Sciences ; Strategic Priority Research Program on Space Science, Chinese Academy of Sciences ; JSPS KAKENHI ; JSPS KAKENHI ; JSPS KAKENHI ; JSPS KAKENHI ; Natural Science Foundation of China ; Natural Science Foundation of China ; Natural Science Foundation of China ; Natural Science Foundation of China ; Strategic Priority Research Program on Space Science, Chinese Academy of Sciences ; Strategic Priority Research Program on Space Science, Chinese Academy of Sciences ; Strategic Priority Research Program on Space Science, Chinese Academy of Sciences ; Strategic Priority Research Program on Space Science, Chinese Academy of Sciences ; JSPS KAKENHI ; JSPS KAKENHI ; JSPS KAKENHI ; JSPS KAKENHI ; Natural Science Foundation of China ; Natural Science Foundation of China ; Natural Science Foundation of China ; Natural Science Foundation of China ; Strategic Priority Research Program on Space Science, Chinese Academy of Sciences ; Strategic Priority Research Program on Space Science, Chinese Academy of Sciences ; Strategic Priority Research Program on Space Science, Chinese Academy of Sciences ; Strategic Priority Research Program on Space Science, Chinese Academy of Sciences ; JSPS KAKENHI ; JSPS KAKENHI ; JSPS KAKENHI ; JSPS KAKENHI
源URL[http://ir.iggcas.ac.cn/handle/132A11/108426]  
专题地质与地球物理研究所_中国科学院地球与行星物理重点实验室
通讯作者Lin, Yangting
作者单位1.Natl Inst Polar Res, Tokyo 1908518, Japan
2.Chinese Acad Sci, Inst Geol & Geophys, Key Lab Earth & Planetary Phys, Beijing 100029, Peoples R China
3.Chinese Acad Sci, Natl Space Sci Ctr, State Key Lab Space Weather, Beijing 100190, Peoples R China
推荐引用方式
GB/T 7714		 Xu, Yuchen,Lin, Yangting,Hao, Jialong,et al. Abundant presolar silicates of the CM chondrite Asuka 12169: Implications for the thermal and aqueous alteration of the CM parent body[J]. GEOCHIMICA ET COSMOCHIMICA ACTA,2022,334:45-64.
APA Xu, Yuchen.,Lin, Yangting.,Hao, Jialong.,Kimura, Makoto.,Hu, Sen.,...&Zou, Yongliao.(2022).Abundant presolar silicates of the CM chondrite Asuka 12169: Implications for the thermal and aqueous alteration of the CM parent body.GEOCHIMICA ET COSMOCHIMICA ACTA,334,45-64.
MLA Xu, Yuchen,et al."Abundant presolar silicates of the CM chondrite Asuka 12169: Implications for the thermal and aqueous alteration of the CM parent body".GEOCHIMICA ET COSMOCHIMICA ACTA 334(2022):45-64.

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来源：地质与地球物理研究所

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