同位素组成的愤由广泛的蒸发和部分再冷凝控制
Baoliang Wang1, Frederic Moynier1, Yan Hu1
1Institut de Physique du Globe de Paris, Université Paris Cité, CNRS, Paris 75005, France.
概括
昂格里特显示比其他行星体更轻的鲁比 (Rb) 同位素,表明一个独特的形成过程. 这支持了一个模型,在这个模型中,蒸发和凝结都影响了早期太阳系中挥发性元素的分布.
科学领域:
- 行星科学 行星科学
- 太空化学 太空化学
- 同位素地球化学 同位素地球化学
背景情况:
- 行星小物显示中度挥发性元素 (MVE) 的变量耗尽.
- 用更重的MVE同位素进行同位素丰富通常与通过蒸发的挥发性损失有关.
- 酸盐是异常的,显示较轻的 (K) 同位素,表明凝结过程.
研究的目的:
- 为了研究 (Rb) 的同位素组成的愤怒.
- 为了将愤怒石Rb同位素与其他太阳系天体进行比较.
- 了解早期太阳系中挥发性元素分离的机制.
主要方法:
- 在石中分析Rb同位素成分.
- 石Rb同位素数据与维斯塔,火星和月球的现有数据进行比较.
- 对Rb和K同位素组成的相关性分析.
主要成果:
- 与维斯塔,火星和月球相比,愤怒石表现出较轻的Rb同位素组成.
- 愤怒的母体 (APB) 显示了估计的δ87Rb范围为-1.19‰至-0.67‰.
- 在包括APB在内的陆地行星天体中,Rb和K同位素组成之间存在强烈的相关性.
结论:
- APB的轻Rb同位素组成可能是海阶段近乎完全蒸发后的动力再冷凝的结果.
- 这支持部分再冷凝模型来解释石中的轻Rb和K同位素.
- 结合在一起的Rb-K同位素标志表明挥发性驱动的分化,突出了凝结在塑造行星尺度上的挥发性元素分布中的重要作用.
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