月表太阳风成因水的研究现状和意义

doi:10.11867/j.issn.1001-8166.2018.05.0473

地球科学进展 ›› 2018, Vol. 33 ›› Issue (5): 473 -482. doi: 10.11867/j.issn.1001-8166.2018.05.0473

月表太阳风成因水的研究现状和意义

曾献棣 ^1, ^2, ³, 唐红 ^1, ^3, ^*, 李雄耀 ^1, ³, 欧阳自远 ¹, 王世杰 ⁴

1.中国科学院地球化学研究所月球与行星科学研究中心,贵州贵阳 550081
2.中国科学院大学, 北京 100049
3.中国科学院太空制造技术重点实验室,北京 100094
4.中国科学院地球化学研究所环境地球化学国家重点实验室,贵州贵阳 550081

收稿日期:2018-01-01 修回日期:2018-04-10 出版日期:2018-05-20
通讯作者: 唐红
基金资助:
*国家自然科学基金项目“月表主要硅酸盐矿物中太阳风成因水的实验对比研究”(编号:41773066);中国科学院青年创新促进会资助.

Research Review and Significance of Lunar Water Originated from Solar Wind

Xiandi Zeng ^1, ^2, ³, Hong Tang ^1, ^3, ^*, Xiongyao Li ^1, ³, Ziyuan Ouyang ¹, Shijie Wang ⁴

1.Lunar and Planetary Science Research Center, Institute of Geochemistry, Chinese Academy of Sciences, Guiyang 550081, China
2.University of Chinese Academy of Sciences, Beijing 100049,China
3.Key Laboratory of Space Manufacturing Technology, Chinese Academy of Sciences, Beijing 100094,China
4.State Key Laboratory of Environmental Geochemistry, Institute of Geochemistry, Chinese Academy of Sciences, Guiyang 550081, China

Received:2018-01-01 Revised:2018-04-10 Online:2018-05-20 Published:2018-06-13
Contact: Hong Tang
About author:
First author:Zeng Xiandi(1992-), male, Guangzhou City, Guangdong Province, Master student. Research areas include lunar planetary science.E-mail:zengxiandi@mail.gyig.ac.cn
Supported by:
Project supported by the National Natural Science Foundation of China “Experimental comparison of the solar wind-produced water in lunar main silicates minerals”(No.41773066);Youth Innovation Promotion Association CAS.

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水是生命活动的基础,也是天体演化的重要部分。月球一直被认为是“无水”星体,但这一观点被最新的研究成果推翻。月球遥感红外光谱和Apollo样品分析结果均证实了月球表面能通过太阳风质子与月壤矿物相互作用来产生OH甚至是H₂O。为探讨其反应过程,相关理论分析和离子注入模拟实验等研究已逐步开展。但是,目前对于太阳风成因水的成因机制,形成时的影响因素,产生后在月表的赋存、迁移和保留机制仍缺乏系统研究。针对这些问题,未来立足于嫦娥五号样品分析,建立月球表面太阳风成因水的形成和迁移运动的模型将会是推进月球水研究的重要部分。这不仅能为月球水资源开发利用提供线索,还可能为太阳系内其他无大气类地行星水来源和演化研究提供参考。

关键词: 月球水, 太阳风, 红外光谱, 月壤, 离子注入实验

Water plays an important role in the evolution history of terrestrial planets and is also an indispensable resource for space exploration. The moon was used to be thought as “bone-dry”. However, this view was challenged by the latest achievements. Both the infrared remote sensing data and Apollo sample results have shown that some hydroxyl (and even H₂O) can be produced by the reaction between the solar wind proton and regolith mineral on the Moon. A series of theoretical analysis and simulated ion implantation experiments have been carried out to discuss such processes. Many issues related to the solar wind-produced water have not been well understood yet, e.g., the formation mechanism, influencing factors, occurrence state, migration, and retention. To answer these questions, it is necessary to investigate the formation mechanism and migration of solar wind-produced water based on the Change’e-5 returned samples in the future. These studies can not only can provide clues for the exploitation and utilization of water on the Moon, but also help us to understand the origin and evolution of water on other airless terrestrial planets.

Key words: Lunar water, Solar wind, Infrared spectra, Lunar regolith, Ions implantation.

中图分类号:

P691

图1 月表上遥感红外水吸收峰分布
(a)VIMS检测在月表不同纬度范围的水吸收峰变化 ^{[

11
]};(b)M ³检测3 μm吸收峰主要在月球极地区域分布 ^{[

12
]};(c)Deep Impact检测2.8 μm吸收峰在北半球月面含量变化图 ^{[

13
]}

Fig.1 Infrared remote sensing of water absorption peaks on lunar surface
(a) Varying water absorbance distribute on lunar surface in different latitudes from VIMS ^{[

11
]}; (b) Measured 3 μm absorption strength on the polar region of the moon from M ^{3[

12
]}; (c) The strength of the continuum-removed 2.8 μm hydration feature on lunar surface of the Northern Hemisphere from the Deep Impact ^{[

13
]}

图2 对比1/4天内月海和高地区域在不同纬度和不同时间的水吸收峰变化 ^{[

13
]}
(a)不同纬度月海区域的水吸收峰变化;(b)不同纬度高地区域的水吸收峰变化;(c)月海区域在不同时间的水吸收峰变化; (d)高地区域在不同时间的水吸收峰变化;(e)1,2,3,9,M为月海区域,5,6,7,8,H为高地区域

Fig.2 Comparisons of mare and highland terrains as a function of latitude and time of day as observed over a quarter of a lunar day ^{[

13
]}
(a)Variation of water absorption in mare region at different latitude;(b)Variation of water absorption in highland region at different latitude; (c)Variation of water absorption in mare region at different time;(d)Variation of water absorption in highland region at different time;(e)1, 2, 3, 9, M for mare region, 5,6,7,8, H for highland region

Fig.3 FTIR spectra and SIMS data of two agglutinates ^{[

20
]}
δD(‰)=[(D/H) _measured/(D/H) _standard-1]×1 000,(D/H) _standard=1.5576×10 ^-4; ppm为×10 ^-6

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