早期月球的形成推断来自哈夫尼-黄系统学
Maxwell M Thiemens1, Peter Sprung1,2, Raúl O C Fonseca1
1Institut für Geologie und Mineralogie, Universität zu Köln, Germany.
概括
月球是在太阳系形成后大约5000万年形成的. 这种早期形成解释了月球样本中过量的-182 (182W),挑战了关于晚期积累的先前理论.
科学领域:
- 地质化学 地质化学
- 行星科学 行星科学
- 太空化学 太空化学
背景情况:
- 月球年龄的估计差异很大,影响我们对地球起源的理解.
- 一个关键的辩论集中在与地球相比,酸盐月球中-182 (182W) 的丰度更高.
- 这种差异以前被归因于核心形成后不同程度的晚期积累.
研究的目的:
- 为了调查月球样本中的182W异常的起源.
- 为了精确月球形成撞击的时间表.
- 重新评估晚期积累在月球和地球进化中的作用.
主要方法:
- 使用感应合等离子体质谱学对月球样本进行高精度的微量元素分析.
- 在月球酸盐中测量哈夫/ (Hf/W) 的比率.
- 整合关于分割系数的实验数据.
主要成果:
- 酸盐月球中的Hf/W比率高于大量的酸盐地球.
- 观察到的182W的过量与短命同位素哈夫-182 (182Hf) 的衰变相一致.
- 182Hf仅存在于太阳系形成的前6000万年.
结论:
- 月球很早就形成了,大约在太阳系形成后的5000万年.
- 月球酸盐中182W的过剩是由放射性衰变解释的,而不是晚期积累.
- 这一发现为月球形成撞击和地球早期历史的时间提供了更精确的约束.
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