Light noble gases in 11 achondrites: Cosmic ray exposure ages, gas retention ages, and preatmospheric sizes
文献类型：期刊论文
| 作者 | Smith, Thomas1,5; He, Huaiyu1,2,3,5; Li, Shijie4; Su, Fei1 |
| 刊名 | METEORITICS & PLANETARY SCIENCE
 |
| 出版日期 | 2023-10-18 |
| 页码 | 20 |
| ISSN号 | 1086-9379 |
| DOI | 10.1111/maps.14085 |
| 英文摘要 | We report light noble gas (He, Ne, and Ar) concentrations and isotopic ratios in 11 achondrites, Tafassasset (unclassified primitive achondrite), Northwest Africa (NWA) 12934 (angrite), NWA 12573 (brachinite), Jiddat al Harasis (JaH) 809 (ureilite), NWA 11562 (ungrouped achondrite), four lodranites (NWA 11901, NWA 7474, NWA 6685, and NWA 6484), NWA 2871 (acapulcoite), and Sahara 02029 (winonaite), most of which have not been previously studied for noble gases. We discuss their noble gas isotopic composition, determine their cosmogenic nuclide content, and systematically calculate their cosmic ray exposure (CRE) and gas retention ages. In addition, we estimate their preatmospheric radii and preatmospheric masses based on the shielding parameter (Ne-22/Ne-21)(cos). None of the studied meteorites shows evidence of contribution from solar cosmic rays (SCRs). JaH 809 and NWA 12934 show evidence of He-3 diffusive losses of >90% and 40%, respectively. The winonaite Sahara 02029 has lost most of its noble gases, either during or before analysis. The average CRE age of Tafassasset of similar to 49 Ma is lower than that reported by Patzer et al. (2003), but is consistent with it within the uncertainties; this confirms that Tafassasset and CR chondrites are not source paired, CR chondrites having CRE ages from 1 to 25 Ma (Herzog & Caffee, 2014). The ureilite JaH 809 has a CRE age of similar to 5.4 Ma, which falls into the typical range of exposure ages for ureilites; the angrite NWA 12934 has a CRE age of similar to 49 Ma, which is within the main range of exposure ages reported for angrites (0.2-56 Ma). We calculate a CRE age of similar to 2.4 Ma for the brachinite NWA 12573, which falls into a possible "cluster" in the brachinite CRE age histogram around similar to 3 Ma. Three lodranites (NWA 11901, NWA 7474, and NWA 6685) have CRE ages higher than the average CRE ages of lodranites measured so far, NWA 11901 and NWA 6685 having CRE ages far higher than the CRE age already reported by Li et al. (2019) on NWA 8118. The measured K-40-Ar-40 gas retention ages fit well into established systematics. The gas retention age of Tafassasset is consistent, within respective uncertainties, with that previously calculated by Patzer et al. (2003). Our study indicates that Tafassasset originates from a meteoroid with a preatmospheric radius of similar to 20 cm, however discordant with the radius of similar to 85 cm inferred in a previous study (Patzer et al., 2003). |
| WOS关键词 | DIFFERENTIATED ACHONDRITES ; CHEMICAL-COMPOSITION ; MARTIAN METEORITES ; ANGRITE ; ACAPULCOITES ; HISTORY ; PETROGRAPHY ; MINERALOGY ; LODRANITES ; CHEMISTRY |
| 资助项目 | This work has been supported through the National Key Ramp;D Program of China #2020YFE0202100. Additionally, this work has been supported through the SKL-K201802 funding grant from the State Key Laboratory of Lithospheric Evolution, IGGCAS, Beijing, the s[2020YFE0202100] ; This work has been supported through the National Key Ramp;D Program of China #2020YFE0202100. Additionally, this work has been supported through the SKL-K201802 funding grant from the State Key Laboratory of Lithospheric Evolution, IGGCAS, Beijing, the s[SKL-K201802] ; National Key Ramp;D Program of China ; State Key Laboratory of Lithospheric Evolution, IGGCAS[XDB41010205] ; State Key Laboratory of Lithospheric Evolution, IGGCAS[D020302] ; Chinese Academy of Sciences[ZDRW-KT-2019-5-5] ; Key Deployment Projects of Chinese Academy of Sciences |
| WOS研究方向 | Geochemistry & Geophysics |
| 语种 | 英语 |
| 出版者 | WILEY |
| WOS记录号 | WOS:001091043300001 |
| 资助机构 | This work has been supported through the National Key Ramp;D Program of China #2020YFE0202100. Additionally, this work has been supported through the SKL-K201802 funding grant from the State Key Laboratory of Lithospheric Evolution, IGGCAS, Beijing, the s ; This work has been supported through the National Key Ramp;D Program of China #2020YFE0202100. Additionally, this work has been supported through the SKL-K201802 funding grant from the State Key Laboratory of Lithospheric Evolution, IGGCAS, Beijing, the s ; This work has been supported through the National Key Ramp;D Program of China #2020YFE0202100. Additionally, this work has been supported through the SKL-K201802 funding grant from the State Key Laboratory of Lithospheric Evolution, IGGCAS, Beijing, the s ; This work has been supported through the National Key Ramp;D Program of China #2020YFE0202100. Additionally, this work has been supported through the SKL-K201802 funding grant from the State Key Laboratory of Lithospheric Evolution, IGGCAS, Beijing, the s ; National Key Ramp;D Program of China ; National Key Ramp;D Program of China ; National Key Ramp;D Program of China ; National Key Ramp;D Program of China ; State Key Laboratory of Lithospheric Evolution, IGGCAS ; State Key Laboratory of Lithospheric Evolution, IGGCAS ; State Key Laboratory of Lithospheric Evolution, IGGCAS ; State Key Laboratory of Lithospheric Evolution, IGGCAS ; Chinese Academy of Sciences ; Chinese Academy of Sciences ; Chinese Academy of Sciences ; Chinese Academy of Sciences ; Key Deployment Projects of Chinese Academy of Sciences ; Key Deployment Projects of Chinese Academy of Sciences ; Key Deployment Projects of Chinese Academy of Sciences ; Key Deployment Projects of Chinese Academy of Sciences ; This work has been supported through the National Key Ramp;D Program of China #2020YFE0202100. Additionally, this work has been supported through the SKL-K201802 funding grant from the State Key Laboratory of Lithospheric Evolution, IGGCAS, Beijing, the s ; This work has been supported through the National Key Ramp;D Program of China #2020YFE0202100. Additionally, this work has been supported through the SKL-K201802 funding grant from the State Key Laboratory of Lithospheric Evolution, IGGCAS, Beijing, the s ; This work has been supported through the National Key Ramp;D Program of China #2020YFE0202100. Additionally, this work has been supported through the SKL-K201802 funding grant from the State Key Laboratory of Lithospheric Evolution, IGGCAS, Beijing, the s ; This work has been supported through the National Key Ramp;D Program of China #2020YFE0202100. Additionally, this work has been supported through the SKL-K201802 funding grant from the State Key Laboratory of Lithospheric Evolution, IGGCAS, Beijing, the s ; National Key Ramp;D Program of China ; National Key Ramp;D Program of China ; National Key Ramp;D Program of China ; National Key Ramp;D Program of China ; State Key Laboratory of Lithospheric Evolution, IGGCAS ; State Key Laboratory of Lithospheric Evolution, IGGCAS ; State Key Laboratory of Lithospheric Evolution, IGGCAS ; State Key Laboratory of Lithospheric Evolution, IGGCAS ; Chinese Academy of Sciences ; Chinese Academy of Sciences ; Chinese Academy of Sciences ; Chinese Academy of Sciences ; Key Deployment Projects of Chinese Academy of Sciences ; Key Deployment Projects of Chinese Academy of Sciences ; Key Deployment Projects of Chinese Academy of Sciences ; Key Deployment Projects of Chinese Academy of Sciences ; This work has been supported through the National Key Ramp;D Program of China #2020YFE0202100. Additionally, this work has been supported through the SKL-K201802 funding grant from the State Key Laboratory of Lithospheric Evolution, IGGCAS, Beijing, the s ; This work has been supported through the National Key Ramp;D Program of China #2020YFE0202100. Additionally, this work has been supported through the SKL-K201802 funding grant from the State Key Laboratory of Lithospheric Evolution, IGGCAS, Beijing, the s ; This work has been supported through the National Key Ramp;D Program of China #2020YFE0202100. Additionally, this work has been supported through the SKL-K201802 funding grant from the State Key Laboratory of Lithospheric Evolution, IGGCAS, Beijing, the s ; This work has been supported through the National Key Ramp;D Program of China #2020YFE0202100. Additionally, this work has been supported through the SKL-K201802 funding grant from the State Key Laboratory of Lithospheric Evolution, IGGCAS, Beijing, the s ; National Key Ramp;D Program of China ; National Key Ramp;D Program of China ; National Key Ramp;D Program of China ; National Key Ramp;D Program of China ; State Key Laboratory of Lithospheric Evolution, IGGCAS ; State Key Laboratory of Lithospheric Evolution, IGGCAS ; State Key Laboratory of Lithospheric Evolution, IGGCAS ; State Key Laboratory of Lithospheric Evolution, IGGCAS ; Chinese Academy of Sciences ; Chinese Academy of Sciences ; Chinese Academy of Sciences ; Chinese Academy of Sciences ; Key Deployment Projects of Chinese Academy of Sciences ; Key Deployment Projects of Chinese Academy of Sciences ; Key Deployment Projects of Chinese Academy of Sciences ; Key Deployment Projects of Chinese Academy of Sciences ; This work has been supported through the National Key Ramp;D Program of China #2020YFE0202100. Additionally, this work has been supported through the SKL-K201802 funding grant from the State Key Laboratory of Lithospheric Evolution, IGGCAS, Beijing, the s ; This work has been supported through the National Key Ramp;D Program of China #2020YFE0202100. Additionally, this work has been supported through the SKL-K201802 funding grant from the State Key Laboratory of Lithospheric Evolution, IGGCAS, Beijing, the s ; This work has been supported through the National Key Ramp;D Program of China #2020YFE0202100. Additionally, this work has been supported through the SKL-K201802 funding grant from the State Key Laboratory of Lithospheric Evolution, IGGCAS, Beijing, the s ; This work has been supported through the National Key Ramp;D Program of China #2020YFE0202100. Additionally, this work has been supported through the SKL-K201802 funding grant from the State Key Laboratory of Lithospheric Evolution, IGGCAS, Beijing, the s ; National Key Ramp;D Program of China ; National Key Ramp;D Program of China ; National Key Ramp;D Program of China ; National Key Ramp;D Program of China ; State Key Laboratory of Lithospheric Evolution, IGGCAS ; State Key Laboratory of Lithospheric Evolution, IGGCAS ; State Key Laboratory of Lithospheric Evolution, IGGCAS ; State Key Laboratory of Lithospheric Evolution, IGGCAS ; Chinese Academy of Sciences ; Chinese Academy of Sciences ; Chinese Academy of Sciences ; Chinese Academy of Sciences ; Key Deployment Projects of Chinese Academy of Sciences ; Key Deployment Projects of Chinese Academy of Sciences ; Key Deployment Projects of Chinese Academy of Sciences ; Key Deployment Projects of Chinese Academy of Sciences |
| 源URL | [http://ir.iggcas.ac.cn/handle/132A11/110715]  |
| 专题 | 地质与地球物理研究所_岩石圈演化国家重点实验室 |
| 通讯作者 | Smith, Thomas; He, Huaiyu |
| 作者单位 | 1.Chinese Acad Sci, Inst Geol & Geophys, State Key Lab Lithospher Evolut, Beijing, Peoples R China 2.Chinese Acad Sci, Inst Earth Sci, Beijing, Peoples R China 3.Univ Chinese Acad Sci, Coll Earth & Planetary Sci, Beijing, Peoples R China 4.Chinese Acad Sci, Inst Geochem, Ctr Lunar & Planetary Sci, Guiyang, Peoples R China 5.Chinese Acad Sci, Inst Geol & Geophys, State Key Lab Lithospher Evolut, Beijing 100029, Peoples R China |
| 推荐引用方式 GB/T 7714 | Smith, Thomas,He, Huaiyu,Li, Shijie,et al. Light noble gases in 11 achondrites: Cosmic ray exposure ages, gas retention ages, and preatmospheric sizes[J]. METEORITICS & PLANETARY SCIENCE,2023:20. |
| APA | Smith, Thomas,He, Huaiyu,Li, Shijie,&Su, Fei.(2023).Light noble gases in 11 achondrites: Cosmic ray exposure ages, gas retention ages, and preatmospheric sizes.METEORITICS & PLANETARY SCIENCE,20. |
| MLA | Smith, Thomas,et al."Light noble gases in 11 achondrites: Cosmic ray exposure ages, gas retention ages, and preatmospheric sizes".METEORITICS & PLANETARY SCIENCE (2023):20. |
入库方式： OAI收割
来源：地质与地球物理研究所
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