History and Evolution of Volatiles in the Earth-Moon System

地月系统挥发物的历史和演化

• 批准号: 2131636
• 金额: --
• 依托单位: The Open University
• 依托单位国家: 英国
• 项目类别: Studentship
• 财政年份: 2018
• 资助国家: 英国
• 起止时间: 2018 至 无数据
• 项目状态: 已结题
• 来源: https://gtr.ukri.org/projects?ref=studentship-2131636
• 关键词: History; Evolution; Volatiles; Earth; Moon

Recent research on lunar samples has confirmed significant presence of water and other volatiles in the Moon (e.g., Hauri et al., 2017). These findings are being used to revise Moon formation models and transform our understanding of the sources and timing of delivery of volatiles to the Earth-Moon system during earliest periods of the Solar System history (Barnes et al., 2016a).Much of the lunar volatiles research has been carried out in-situ on melt inclusions, nominally anhydrous minerals and the mineral apatite that contains water (as hydroxyl) and other volatile elements (e.g., F, Cl, S) in its crystal structure. Of these, apatite is the most common volatile-bearing phase across a wide variety of lunar rocks. The H and Cl isotope signatures of lunar apatite reveal complex interplay between planetary processes (e.g., magma degassing, cosmic ray spallation, impact-induced metasomatism) that need to be better understood in order to identify and quantify different sources of volatiles to the Earth-Moon system (Fig. 1). Currently, an in-depth study linking petrography with in-situ geochemical measurements for volatiles in planetary samples is lacking. This approach is key to interpreting existing and any new dataset for constraining various solar system processes and evaluate the role asteroids and comets in delivering water to the Earth-Moon system (e.g., Marty, 2012).

最近对月球样本的研究证实了月球中存在大量的水和其他挥发物（例如，Hauri等人，2017年）。这些发现正在被用来修正月球形成模型，并改变我们对太阳系历史早期挥发物向地月系统输送的来源和时间的理解（巴恩斯等人，大部分月球挥发物研究都是在熔融包裹体上进行的，名义上是无水矿物和含有水（作为羟基）和其他挥发性元素（例如，F，Cl，S）的晶体结构。其中，磷灰石是各种月球岩石中最常见的含挥发物相。月球磷灰石的氢和氯同位素特征揭示了行星过程之间复杂的相互作用（例如，岩浆脱气、宇宙射线散射、撞击诱导的交代作用），这些都需要更好地理解，以便确定和量化地月系统挥发物的不同来源（图1）。目前，缺乏将岩石学与行星样品中挥发物的现场地球化学测量联系起来的深入研究。这种方法是解释现有和任何新数据集的关键，用于约束各种太阳系过程，并评估小行星和彗星在向地月系统提供水方面的作用（例如，Marty，2012）。