最早的行星体上的晚期积聚是由高度 siderophile 元素所揭示的
Christopher W Dale1, Kevin W Burton, Richard C Greenwood
1Department of Earth Sciences, Durham University, Durham DH1 3LE, UK. christopher.dale@durham.ac.uk
概括
晚期积聚的体物质解释了行星地幔中高度 siderophile 元素 (HSEs) 的丰富性. 这种过程在所有差异化物体中都是常见的,氧化状态控制着HSE分布.
科学领域:
- 行星科学 行星科学
- 地质化学 地质化学
- 太空化学 太空化学
背景情况:
- 陆地行星地幔中高度 siderophile 元素 (HSEs) 的丰富性是由核心形成后的体物质的晚期积累解释的.
- 以前的研究集中在像地球,月球和火星这样的大型天体上.
研究的目的:
- 为了研究较小的行星类物质中的HSE丰度.
- 为了确定状物质的晚期积累是否是差异化物体的普遍过程.
- 了解控制行星地幔中HSE分布的因素.
主要方法:
- 在较小的行星体中分析高度 siderophile 元素 (HSE) 的丰度.
- 对HSE比例与体材料进行比较.
- 模拟母体大小和氧化状态对HSE分布的影响.
主要成果:
- 较小的行星类星体也表现出高的HSE丰度,其比例高于体.
- 晚期积聚的体物质发生在一个很长的时间框架 (太阳系形成后的5至1.5亿年).
- 父母体的大小影响绝对的HSE丰度,而氧化状态是HSE混合到化物地幔的主要控制.
结论:
- 晚期添加的体物质是所有差异化行星和行星小行星的共同过程.
- 一个体的氧化状态是决定其化的最终HSE含量的一个关键因素.
- 了解这些过程,可以了解太阳系中岩石体的早期演变.
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