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摘要:
为研究太阳风成因水在月表低纬度地区的分布特征，本文对中国科学院地质与地球物理研究所博物馆珍藏的一份Apollo 11月壤样品开展了单颗粒原位纳米离子探针H同位素和水含量深度剖面分析。结果表明月壤颗粒表层（< 200nm）具有较高的水含量（剖面最大水含量变化范围为0.35%~1.59%，平均值为0.82%），该结果与前人对Apollo样品的报导类似。除一颗斜长石的H同位素组成（δD=-262‰）落在月幔范围内，其余颗粒表层均非常贫D（δD变化范围为-987‰~-642‰）。该强烈贫D的同位素组成与太阳风一致，完全不同于地球大气水，不仅证明这些样品的月球来源，并且主要是太阳风注入的贡献。矿物颗粒之间的水含量和δD值变化，很可能与太阳风注入后的扩散丢失程度不同有关。另外，我们观察到橄榄石、单斜辉石和长石的水含量剖面比较类似，整体呈现随深度逐渐递减的趋势。相比之下，玻璃质颗粒的水含量剖面呈现随深度先上升再降低的峰形特征，峰位在25~43nm深度。这两者之间的差异很可能跟H在矿物和玻璃中的扩散速率、辐射损伤层等的差异有关。本项研究也证明，即使对于H这样易于受地球污染的元素，在普通条件下（北京、瓶中密封）经过长达50多年的时间，仍能很好地保存注入月壤颗粒中的太阳风信息。但是低温、干燥和真空/惰性气体环境仍是长期保存的有利条件。
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关键词:
- 阿波罗11号 /
- 月壤 /
- 太阳风 /
- 水含量及氢同位素深度分析 /
- 月球低纬度地区
Abstract:To investigate the distribution of solar-wind implanted H in the low latitude regions of the lunar surface, we carried out NanoSIMS depth-profiling measurements of H isotope and water content on Apollo 11 soils that were stored in the Geological Museum, Institute of Geology and Geophysics, Chinese Academy of Sciences. The results show that the surface of all lunar grains (< 200nm) has a high water content (the maximum water content varying from 0.35% to 1.59%), which is similar to the results of previous studies on Apollo 11 samples. Except for one plagioclase (A11-021-1) whose surface H isotope composition (δD) is -262‰, the other grains have very low δD values ranging from -987‰ to -642‰. These characteristics indicate that the high water content in the surface layer of lunar grains is the result of solar-wind implantation rather than terrestrial contamination. The different water contents and δD values may be caused by H diffusion after initial solar-wind implantation. In addition, we find that the water-content depth profiles of olivine, clinopyroxene and plagioclase are similar, and their water contents gradually decrease with increasing depth. By contrast, two glassy grains show simple bell-shaped water-content distributions as a function of depth that peak ca.25~43nm below the grain surface. Such a phenomenon may be related to the difference of H diffusion rate in crystalline grain and glass and the difference of the damaged layers. As a specific study, this work also suggests that low temperature, dry and vacuum/inert gas environments are still favorable conditions for long-term preservation of extraterrestrial samples.
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Key words:
- Apollo 11 /
- Lunar regolith /
- Solar wind /
- Water content and H isotopes /
- Low latitude
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图 1
Apollo样品水含量深度剖面前人研究工作(数据来自Leich et al., 1973, 1974; Hashizume et al., 2000)
Figure 1.
The water-content depth profiles of Apollo lunar grains in previous studies (data from Leich et al., 1973, 1974; Hashizume et al., 2000)
图 2
挑选的Apollo 11月壤颗粒镜下照片(a)和月壤颗粒压铟后的背散射图像(b)
Figure 2.
The microscope photo for the selected Apollo 11 grains (a) and the back-scattered electron image (b)
图 3
样品A11-011-1的原始O、H和D计数剖面变化(a)和水含量换算曲线(b)
Figure 3.
The O, H and D depth profile of sample A11-011-1 (a) and the water-content calibration line determined by the apatite and silicate glass standards (b)
图 4
Apollo 11月壤颗粒二次电子图像
Figure 4.
The secondary electron images of the Apollo 11 grains
图 5
Apollo 11月壤颗粒水含量剖面随深度变化结果
Figure 5.
The water-content versus depth for the Apollo 11 lunar grains
图 6
斜长石A11-021-1的H、O、C和C/O深度剖面变化
Figure 6.
The H, O, C and C/O depth profiles for sample A11-021-1
图 7
Apollo 11月壤颗粒D/H比值与其它储库H同位素组成对比关系图(底图中月球、地球、球粒陨石、IDP、彗星等储库H同位素组成来自Liu et al., 2012)
Figure 7.
The D/H ratios for the Apollo 11 lunar grains, in comparison with other reservoirs (the data for Earth, Moon, chondrites, IDP and comets from Liu et al., 2012)
表 1
Apollo 11月壤颗粒水含量特征和H同位素组成
Table 1.
The water content and hydrogen isotopic compositions of the Apollo 11 lunar grains
样品号 颗粒类型 最大水含量
(%)δD in 100nm
(‰)δD误差(1σ) 900~1000nm深度水含量
(×10-6)峰位置
(nm)A11-005-1 玻璃 0.74 -868 19 1630 ~43 A11-005-2 玻璃 0.70 -932 16 940 ~33 A11-016-1 玻璃 0.90 -847 21 610 — A11-016-2 玻璃 1.59 -732 26 570 — A11-017-1 玻璃 0.94 -987 5 260 ~25 A11-011-1 斜长石 0.66 -845 26 180 — A11-019-2 斜长石 0.72 -642 52 230 — A11-021-1 斜长石 0.35 -262 77 270 — A11-018-1 橄榄石 1.17 -929 24 200 — A11-012-1 单斜辉石 0.86 -894 18 70 — A11-020-1 单斜辉石 0.61 -794 31 490 — A11-020-2 单斜辉石 0.57 -760 35 360 — 注：颗粒类型由拉曼光谱和扫描电镜能谱分析获得.根据对嫦娥五号月壤颗粒的分析测试，每层剥蚀厚度约1nm左右.由于每层所获得的D计数非常低，本次研究计算了前100层累加值的H同位素组成.δD in 100nm (‰)是由前100层所获得的D/H比值计算得来，误差为统计误差.900~1000nm深度水含量(×10-6): 水含量在900~1000nm深度的平均值(样品A11-020-1为统计500~600nm深度范围) 
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