書誌事項
- 公開日
- 2017-08-15
- 権利情報
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- https://creativecommons.org/licenses/by/4.0
- https://creativecommons.org/licenses/by/4.0
- DOI
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- 10.1038/s41467-017-00293-1
- 公開者
- Springer Science and Business Media LLC
説明
<jats:title>Abstract</jats:title><jats:p>Early Solar System planetesimal thermal models predict the heating of the chondritic protolith and the preservation of a chondritic crust on differentiated parent bodies. Petrological and geochemical analyses of chondrites have suggested that secondary alteration phases formed at low temperatures (<300 °C) by fluid-rock interaction where reduced and oxidized Vigarano type Carbonaceous (CV) chondrites witness different physicochemical conditions. From a thermodynamical survey of Ca-Fe-rich secondary phases in CV3 chondrites including silica activity (<jats:italic>a</jats:italic>SiO<jats:sub>2</jats:sub>), here we show that the classical distinction between reduced and oxidized chondrites is no longer valid and that their Ca-Fe-rich secondary phases formed in similar reduced conditions near the iron-magnetite redox buffer at low <jats:italic>a</jats:italic>SiO<jats:sub>2</jats:sub> (log<jats:italic>(a</jats:italic>SiO<jats:sub>2</jats:sub>) <−1) and moderate temperature (210–610 °C). The various lithologies in CV3 chondrites are inferred to be fragments of an asteroid percolated heterogeneously via porous flow of hydrothermal fluid. Putative ‘onion shell’ structures are not anymore a requirement for the CV parent body crust.</jats:p>
収録刊行物
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- Nature Communications
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Nature Communications 8 (1), 261-, 2017-08-15
Springer Science and Business Media LLC
