在地球和火星的核心形成过程中氧气的分割
David C Rubie1, Christine K Gessmann, Daniel J Frost
1Bayerisches Geoinstitut, University of Bayreuth, D-95444 Bayreuth, Germany. dave.rubie@uni-bayreuth.de
Nature
|May 7, 2004
概括
地球和火星的核心形成因液体铁中取决于温度的氧气溶解度而不同. 地球较高的温度提取了更多的氧化铁 (FeO),使火星的地幔更丰富.
科学领域:
- 行星科学 行星科学
- 地质化学 地质化学
- 地球科学 地球科学 地球科学
背景情况:
- 陆地行星中核心的形成涉及金属酸盐的分离,可能在岩海洋中.
- 现有的模型不能完全解释地球和火星地幔的组成差异,特别是氧化铁 (FeO) 含量和核心质量分数.
研究的目的:
- 为了解释观察到的地球 (大约. 8重%的FeO) 和火星的 (大约. 18重量% FeO) 的地幔组成.
- 与地球相比,火星核心的质量分数较小.
主要方法:
- 研究了地球和火星深层岩海洋中的核心形成过程.
- 应用了一个基于氧气在液体铁合金中的温度依赖溶解度的模型.
主要成果:
- 温度升高提高了液体铁中的氧气溶解度,促进了从酸盐岩中提取FeO.
- 地球上更热的岩海洋 (1,2002,000公里深) 提取了大量的FeO,导致地幔含FeO较少.
- 火星较冷的岩海洋经历了极少的FeO提取,导致其特有的富含FeO的地幔.
结论:
- 液体铁中取决于温度的氧气溶解度是控制行星核心形成和地幔组成的关键因素.
- 从地球的岩海洋中提取的FeO可能影响了最下层地幔的化学异质性和核心的轻元素预算.
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