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不论是接触式还是非接触式探测,月壤是最直接的探测目标。因此准确了解月壤的物理性质对采用合适的探测手段及相关影响因素分析具有关键的作用。
1)力学性质
月壤主要由硅酸盐矿物和玻璃质组成,两者之间的宏观力学性质较接近。参考静压条件下不同孔隙比月壤样品的压缩系数[23],可推测出极区月壤孔隙率在51% ~ 35%之间时,对应孔隙比1.04 ~ 0.54,平均压缩系数3 ~ 20,承载力7~ 55 kPa,总体上与月海的月壤基本相当。内聚力和内摩擦角随深度的增大呈现升高的趋势,表层月壤的内聚力在0.44 ~ 0.62 kPa之间,内摩擦角41° ~ 43°之间;30 ~ 60 cm处两者分别在2.4 ~ 3.8 kPa和52° ~ 55°之间。
2)热学性质
太阳系内许多天体无大气,月球、水星和小行星,其表面由于缺少大气层的保护,受到大量流星体撞击后覆盖一层颗粒较小的风化层。这层风化物的热学性质是了解天体表面热状态和地质过程的基本参数。热导率是衡量天体表层风化物热传导能力的重要参数。在真空环境下,粉末物质的热导率(如月壤)比岩石的热导率低几个数量级。热导率除受密度的影响之外,也会受气压、温度、颗粒大小等因素的影响[67-68]。在0.1 torr以下热导率随气压的变化非常小,之后随气压的增大而增大[69-70]。极区月壤斜长石含量较高,而斜长石热导率比辉石和橄榄石小,参照Apollo 16月壤,推测出在100 ~ 400 K内极区月壤热导率(0.5~1.5)×10–3W·m–1·K–1间;随着深度的增加,由于密度增大热导率也随之增大,其与月海月壤变化趋势基本一致。
3)电学性质
电导率是度量电流在物质中传输的难易程度,月表硅酸盐属于典型的低电导物质。电导率是影响月尘带电浮扬防护、利用月球的电磁测深数据推导月球内部的温度剖面及月球矿产资源选冶等所需要的关键参数。
月壤电导率随温度的变化表现出非晶质特征,表明月表的月壤受到了强烈辐射损伤。Apollo 15月壤样品分析结果表明电导率随温度的变化符合指数关系[71],Apollo 16月岩样品的电导率随温度的变化关系与月壤相似。月表物质的电导率除受月表温度控制外,还受月表太阳辐射的影响。太阳辐射可大大改变月表物质的电导率,使月表物质在太阳晨昏线附近有较大的电荷运动。观测结果表明,黑夜时月表物质的直流电电导率从月壤的10–14ohm/m到月岩的10–9ohm/m不等;当太阳光照射时,月壤和月岩的电导率至少有106ohm/m以上的增加[23]。
介电常数是度量物质保持电荷间距离的能力(即电荷极化)。对于绝对无水的月岩来说,其矿物组成、结构和构造是决定其电阻率和复介电常数的主要因素;而对结构松散的月壤来说,复介电常数的影响因素主要包括测试频率、样品密度、测试温度、化学成分等4个方面[71-72]。由于极区钛铁氧化物含量较低,相对月海月壤介电常数也较小,相对介电常数1 ~ 8之间,介电损耗0.001 ~ 2之间,纵向由于组分变化小而呈现很小的变化[23]。Apollo16月球样品的复介电常数测量结果显示,其相对介电常数在1.66 ~ 7.82之间,介电损耗在0.001 ~ 2之间。真空介电常数主要与物质的组分相关,根据极区月壤矿物组成与Apollo16样品类似,因此推测也表现出类似的介电属性。
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月球样品珍贵且稀少,为满足工程探测的大量需求,需要制备相关研究区域的模拟月壤。目前已经公开报道的有3类模拟月壤[73–75]:①典型的月海模拟壤;②典型的高地模拟壤;③南极模拟月壤。本文所关注的是月球南极模拟月壤。
为满足月球南极地区探测的需求,制备月球高地模拟月壤是首要任务。国际上已展开了月球高地模拟壤的工作,并成功模拟出了不同的高地月壤。对于任何模拟月壤应当满足基本的特性:粒径、粒径分布、混合的岩石碎屑、矿物碎屑和玻璃。对于月球高地,超过80%的基岩由钙长岩–苏长岩–橄长岩套组成,而玄武岩仅占基岩的17%左右。目前,国际上普遍以Apollo16样品的综合物性作为高地模拟月壤的参考对象。已经报道的高地模拟壤对比如表1所示。通过对比,NU-LHT-1M/2M模拟壤与Apollo 16样品(64001/64002)的成分最为接近,尤其是钙长石含量最为接近,也是衡量高地模拟壤的关键。
表 1模拟高地月壤与Apollo 16月壤样品成分对比[76]
Table 1.Comparison of mineral composition between lunar highland regolith simulants and Apollo 16 regolith[76]
% 组分 Apollo 16
(64001/64002)NU-LHT-1M NU-LHT-2M OB-1 JSC-1 JSC-1A JSC-1AF FJS-1 MLS-1 岩石碎屑 31.10 — — — 90.90 90.90 91.90 80.20 52.30 玻璃 8.90 22.40 7.20 52.60 — — — 0.50 36.60 粘合集块岩 32.50 29.00 23.50 — — — — — — 斜长岩 23.30 38.80 54.90 43.90 1.50 1.50 3.40 14.10 2.60 钙长石(An%) 95.00 80.00 80.00 75.00 68.00 70.00 70 50.00 47.00 橄榄石 — 2.90 9.50 — 5.60 5.60 4.10 1.10 — 斜辉石 0.60 2.00 4.00 0.10 1.30 1.30 0.40 1.20 2.20 斜方辉石 3.20 4.40 0.20 — — — — — — 尖晶石矿物 0.03 0.05 0.01 0.19 — 0.04 0.02 0.05 0.03 铁硫化物 0.01 — 0.04 — — — — — — 钙–磷酸盐 0.12 — 0.43 — — — — — — 钛铁矿 0.10 0.30 0.20 — — 0.10 — 0.10 1.10 其它 0.01 0.20 0.10 3.10 — 0.50 0.10 2.6 5.20 总计 100.00 100.00 100.00 100.00 100.00 100.00 100.00 100.00 100.00 通过对各个模拟的月壤成分和粒形分布对比,在制备月球高地模拟壤时同样以Apollo16样品为参考对象,但需要注意:①选取原始物料时需要考虑岩石的组成,斜长岩、钙长石(An%)和粘合集块岩的含量;②破碎、研磨时,需要选取合适的方法,控制粒形分布。
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极区模拟月壤制备的准确性对前期工程试验至关重要,分析和对比不同模拟月壤的特征,需要从化学组成、矿物组成和粒径分布这3个基本方面作为模拟月壤制备的标准。
1)化学组成:参考极区LP伽马光谱数据、斜长质月壳组成和Apollo 16月壤分析结果,表2列出了极区月壤的化学组成参考。
表 2不同地区月壤化学组成(百分含量)对比
Table 2.Comparison of lunar regolith chemical composition (in percentage) at different regions
% 化学成分 Apollo 16 月壤* 参考值(3σ) SiO2 45.00 44.3~45.8 TiO2 0.52 0.2~0.8 Al2O3 27.60 24.4~30.8 FeO 4.85 2.6~7.1 MgO 5.46 3.4~7.6 CaO 15.80 14.1~17.5 注:*Apollo 16返回月壤平均成分[77]。 2)矿物组成:主要为斜长石(钙长石),月壤中的斜长石可达70 ~ 80 vol%,橄榄石、辉石和玻璃质的含量小于20 vol%。
3)粒径及分布、热电性质,具体参数见表3。
表 3极区月壤模拟物基础物性参考规范
Table 3.Reference specification of lunar polar regolith simulants
参数 范围 颗粒大小 颗粒直径以小于1 mm为主,绝大部分颗粒直径在
30 µm~1 mm之间,平均粒径140 ~375 μm孔隙度 35% ~ 51% 热导率 (0.5~1.5)×10–3W·m–1·K–1(< 500 Pa) 介电性质 相对介电常数1 ~ 8之间,
介电损耗0.001 ~ 2之间
Review of the Lunar Regolith and Water Ice on the Poles of the Moon
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摘要:月球极区独特的光照条件和表面环境特征是水富集和保存的理想场所,探测永久阴影区内的水冰对科学研究和开发利用月球资源具有重要的意义。综合调研了国际上在月球极区开展的理论研究和遥感探测成果,阐述了极区地质、表面光照条件和热环境特征。介绍了极区月壤和水的形成演化机制及水冰可能的赋存状态。系统梳理了国际上关于极区水冰的探测历程和方法,综合各种探测结果后取得的关于水冰分布特征的认识。根据分析Apollo 16样品后得到的物性、化学、矿物组成和粒径分布基本特征,提出了极区月壤模拟样品制备标准。通过对月球极区探测结果梳理并建立了系统认识极区地质演化的框架,为将来的月球极区月壤和水冰探测提供较为全面的参考。Abstract:Water can be trapped at permanently shadowed regions(PSRs)of the Moon for billions of years due to the extremely low temperatures. Polar exploration targeting water ice can help us understand water evolution and future resource utilization. This study reviews lunar explorations and theoretical studies about the Moon’s pole in past decades. Firstly, we introduce the geological features, illuminating conditions and thermal environment on the poles of the Moon. Secondly, we present the geological evolution of ice-bearing regolith and possible forms of water ice. Thirdly, we summarize all the methods of water detection and water distribution on the Moon. Lastly, we propose a basic standard for producing lunar regolith simulants based on measurements of Apollo samples. This study aims to present a general knowledge of lunar polar geology and provide a reference for future lunar polar exploration.Highlights
● Geological evolution and thermal environments of lunar polar region are reviewed in detail. ● Evolution mechanism and occurrence of water ice at the Moon’s pole are reviewed. ● Lunar polar water explorations are systematically summarized and compared. ● Physical properties including mechanical,thermal and electrical of lunar regolith are summarized. ● A basic standard for producing lunar polar regolith simulants is proposed. -
表 1模拟高地月壤与Apollo 16月壤样品成分对比[76]
Table 1Comparison of mineral composition between lunar highland regolith simulants and Apollo 16 regolith[76]
% 组分 Apollo 16
(64001/64002)NU-LHT-1M NU-LHT-2M OB-1 JSC-1 JSC-1A JSC-1AF FJS-1 MLS-1 岩石碎屑 31.10 — — — 90.90 90.90 91.90 80.20 52.30 玻璃 8.90 22.40 7.20 52.60 — — — 0.50 36.60 粘合集块岩 32.50 29.00 23.50 — — — — — — 斜长岩 23.30 38.80 54.90 43.90 1.50 1.50 3.40 14.10 2.60 钙长石(An%) 95.00 80.00 80.00 75.00 68.00 70.00 70 50.00 47.00 橄榄石 — 2.90 9.50 — 5.60 5.60 4.10 1.10 — 斜辉石 0.60 2.00 4.00 0.10 1.30 1.30 0.40 1.20 2.20 斜方辉石 3.20 4.40 0.20 — — — — — — 尖晶石矿物 0.03 0.05 0.01 0.19 — 0.04 0.02 0.05 0.03 铁硫化物 0.01 — 0.04 — — — — — — 钙–磷酸盐 0.12 — 0.43 — — — — — — 钛铁矿 0.10 0.30 0.20 — — 0.10 — 0.10 1.10 其它 0.01 0.20 0.10 3.10 — 0.50 0.10 2.6 5.20 总计 100.00 100.00 100.00 100.00 100.00 100.00 100.00 100.00 100.00 表 2不同地区月壤化学组成(百分含量)对比
Table 2Comparison of lunar regolith chemical composition (in percentage) at different regions
% 化学成分 Apollo 16 月壤* 参考值(3σ) SiO2 45.00 44.3~45.8 TiO2 0.52 0.2~0.8 Al2O3 27.60 24.4~30.8 FeO 4.85 2.6~7.1 MgO 5.46 3.4~7.6 CaO 15.80 14.1~17.5 注:*Apollo 16返回月壤平均成分[77]。 表 3极区月壤模拟物基础物性参考规范
Table 3Reference specification of lunar polar regolith simulants
参数 范围 颗粒大小 颗粒直径以小于1 mm为主,绝大部分颗粒直径在
30 µm~1 mm之间,平均粒径140 ~375 μm孔隙度 35% ~ 51% 热导率 (0.5~1.5)×10–3W·m–1·K–1(< 500 Pa) 介电性质 相对介电常数1 ~ 8之间,
介电损耗0.001 ~ 2之间 -
[1] MAZARICO E,NEUMANN G A,SMITH D E,et al. Illumination conditions of the lunar polar regions using LOLA topography[J]. Icarus,2011,211(2):1066-1081.doi:10.1016/j.icarus.2010.10.030 [2] GLÄSER P,OBERST J,NEUMANN G A,et al. Illumination conditions at the lunar poles:implications for future exploration[J]. Planetary and Space Science,2018,162:170-178.doi:10.1016/j.pss.2017.07.006 [3] SPEYERER E J,ROBINSON M S. Persistently illuminated regions at the lunar poles:ideal sites for future exploration[J]. Icarus,2013,222(1):122-136.doi:10.1016/j.icarus.2012.10.010 [4] HARUYAMA J,OHTAKE M,MATSUNAGA T,et al. Lack of exposed ice inside lunar south pole shackleton crater[J]. Science,2008,322(5903):938-939.doi:10.1126/science.1164020 [5] NOZETTE S,LICHTENBERG C L,SPUDIS P D,et al. The Clementine bistatic radar experiment[J]. Science,1996,274(5292):1495-1498.doi:10.1126/science.274.5292.1495 [6] FELDMAN W C. Fluxes of fast and epithermal neutrons from lunar prospector:evidence for water ice at the lunar poles[J]. Science,1998,281(5382):1496-1500.doi:10.1126/science.281.5382.1496 [7] PIETERS C M,GOSWAMI J N,CLARK R N,et al. Character and spatial distribution of OH/H2O on the surface of the Moon seen by M3 on Chandrayaan-1[J]. Science,2009,326(5952):568-572.doi:10.1126/science.1178658 [8] SANIN A B,MITROFANOV I G,LITVAK M L,et al. Hydrogen distribution in the lunar polar regions[J]. Icarus,2017,283:20-30.doi:10.1016/j.icarus.2016.06.002 [9] SPUDIS P D,BUSSEY D B J,BALOGA S M,et al. Evidence for water ice on the Moon:results for anomalous polar craters from the LRO Mini-RF imaging radar:evidence for ice on the Moon[J]. Journal of Geophysical Research:Planets,2013,118(10):2016-2029. [10] HAYNE P O,HENDRIX A,SEFTON-NASH E,et al. Evidence for exposed water ice in the Moon’s south polar regions from Lunar Reconnaissance Orbiter ultraviolet albedo and temperature measurements[J]. Icarus,2015,255:58-69.doi:10.1016/j.icarus.2015.03.032 [11] COLAPRETE A,SCHULTZ P,HELDMANN J,et al. Detection of water in the LCROSS ejecta plume[J]. Science,2010,330(6003):463-468.doi:10.1126/science.1186986 [12] 张熇,杜宇,李飞,等. 月球南极探测着陆工程选址建议[J]. 深空探测学报(中英文),2020,7(3):232-240.ZHANG H,DU Y,LI F,et al. Proposals for lunar south polar region soft landing sites selection[J]. Journal of Deep Space Exploration,2020,7(3):232-240. [13] 贾瑛卓,覃朗,徐琳,等. 月球水冰探测[J]. 深空探测学报(中英文),2020,7(3):290-296.JIA Y Z,QIN L,XU L,et al. Lunar water-ice exploration[J]. Journal of Deep Space Exploration,2020,7(3):290-296. [14] WATSON K,MURRAY B C,BROWN H. The behavior of volatiles on the lunar surface[J]. Journal of Geophysical Research,1961,66(9):3033-3045.doi:10.1029/JZ066i009p03033 [15] HODGES R R. Ice in the lunar polar regions revisited[J]. Journal of Geophysical Research,2002,107(E2):5011.doi:10.1029/2000JE001491 [16] SCHORGHOFER N. Migration calculations for water in the exosphere of the Moon:dusk-dawn asymmetry,heterogeneous trapping,and D/H fractionation[J]. Geophysical Research Letters,2014,41(14):4888-4893.doi:10.1002/2014GL060820 [17] ARNOLD J R. Ice in the lunar polar regions[J]. Journal of Geophysical Research,1979,84(B10):5659.doi:10.1029/JB084iB10p05659 [18] LANZEROTTI L J,BROWN W L,JOHNSON R E. Ice in the polar regions of the Moon[J]. Journal of Geophysical Research,1981,86(B5):3949.doi:10.1029/JB086iB05p03949 [19] BARNES J J,KRING D A,TARTÈSE R,et al. An asteroidal origin for water in the Moon[J]. Nature Communications,2016,7(1):11684.doi:10.1038/ncomms11684 [20] LAWRENCE D J. A tale of two poles:Toward understanding the presence,distribution,and origin of volatiles at the polar regions of the Moon and Mercury:polar volatiles at the Moon and Mercury[J]. Journal of Geophysical Research:Planets,2017,122(1):21-52. [21] CANNON K M,BRITT D T. A geologic model for lunar ice deposits at mining scales[J]. Icarus,2020,347:113778.doi:10.1016/j.icarus.2020.113778 [22] CANNON K M,DEUTSCH A N,HEAD J W,et al. Stratigraphy of ice and ejecta deposits at the lunar poles[J]. Geophysical Research Letters,2020,47(21):1-11. [23] HEIKEN G H, VANIMAN D T, FRENCH B M. Lunar sourcebook—a user’s guide to the Moon[M]. New York: Cambridge University Press, 1991. [24] MOLARO J L,BYRNE S,LE J L. Thermally induced stresses in boulders on airless body surfaces,and implications for rock breakdown[J]. Icarus,2017,294:247-261.doi:10.1016/j.icarus.2017.03.008 [25] THOMPSON M S,ZEGA T J,BECERRA P,et al. The oxidation state of nanophase Fe particles in lunar soil:implications for space weathering[J]. Meteoritics & Planetary Science,2016,51(6):1082-1095. [26] TYE A R,FASSETT C I,HEAD J W,et al. The age of lunar south circumpolar craters Haworth,Shoemaker,Faustini,and Shackleton:implications for regional geology,surface processes,and volatile sequestration[J]. Icarus,2015,255:70-77.doi:10.1016/j.icarus.2015.03.016 [27] MARGOT J L. Topography of the lunar poles from radar interferometry:a survey of cold trap locations[J]. Science,1999,284(5420):1658-1660.doi:10.1126/science.284.5420.1658 [28] NODA H,ARAKI H,GOOSSENS S,et al. Illumination conditions at the lunar polar regions by KAGUYA(SELENE) laser altimeter[J]. Geophysical Research Letters,2008,35(24):L24203.doi:10.1029/2008GL035692 [29] BUSSEY D B J,MCGOVERN J A,SPUDIS P D,et al. Illumination conditions of the south pole of the Moon derived using Kaguya topography[J]. Icarus,2010,208(2):558-564.doi:10.1016/j.icarus.2010.03.028 [30] ROSA D D,BUSSEY B,CAHILL J T,et al. Characterisation of potential landing sites for the European Space Agency’s lunar lander project[J]. Planetary and Space Science,2012,74(1):224-246.doi:10.1016/j.pss.2012.08.002 [31] 郝卫峰,李斐,鄢建国,等. 基 于 “嫦 娥 一 号 ”激 光 测 高 数 据 的 月球极区光照条件研究[J]. 地 球 物 理 学 报,2012,55(1):46-52.doi:10.1002/cjg2.1699HAO W F,LI F,YAN J G,et al. Lunar polar ilumination based on Chang′E-1 laser altimeter[J]. Chinese Journal of Geophysics,2012,55(1):46-52.doi:10.1002/cjg2.1699 [32] LIU N,JIN Y Q. Simulation and data analysis of the temperature distribution and variation in the permanent shaded region of the Moon[J]. IEEE Transactions on Geoscience and Remote Sensing,2021,59(4):2962-2972.doi:10.1109/TGRS.2020.3009117 [33] LIU N,JIN Y Q. A real-time model of the seasonal temperature of lunar polar region and data validation[J]. IEEE Transactions on Geoscience and Remote Sensing,2020,58(3):1892-1903.doi:10.1109/TGRS.2019.2950300 [34] PAIGE D A,SIEGLER M A,ZHANG J A,et al. Diviner lunar radiometer observations of cold traps in the Moon’s south polar region[J]. Science,2010,330(6003):479-482.doi:10.1126/science.1187726 [35] PAIGE D A,FOOTE M C,GREENHAGEN B T,et al. The lunar reconnaissance orbiter diviner lunar radiometer experiment[J]. Space Science Reviews,2010,150(1-4):125-160.doi:10.1007/s11214-009-9529-2 [36] WILLIAMS J P. ,GREENHAGEN B T,PAIGE D A,et al. Seasonal polar temperatures on the Moon[J]. Journal of Geophysical Research:Planets,2019,124(10):2505-2521. [37] PIERAZZO E, CHYBA C F. Impact delivery of prebiotic organic matter to planetary surfaces[M]. Berlin, Heidelberg: Springer: 2006, 137-168. [38] MORGAN T H,SHEMANSKY D E. Limits to the lunar atmosphere[J]. Journal of Geophysical Research,1991,96(A2):1351-1367.doi:10.1029/90JA02127 [39] ONG L,ASPHAUGA E I,KORYCANSKYC D,et al. Volatile retention from cometary impacts on the Moon[J]. Icarus,2010,207(2):578-589.doi:10.1016/j.icarus.2009.12.012 [40] MEIER R,OWEN T C,MATTHEWS H E,et al. A determination of the HDO/H2O ratio in comet C/1995 O1 (Hale-Bopp)[J]. Science,1998,279(5352):842-844.doi:10.1126/science.279.5352.842 [41] GEISS J,REEVES H. Deuterium in the solar system[J]. Astronomy and Astrophysics,1981,93:189-199. [42] KERRIDGE J F. What can meteorites tell us about nebular conditions and processes during planetesimal accretion?[J]. Icarus,1993,106(1):135-150.doi:10.1006/icar.1993.1162 [43] HU S,HE H,JI J,et al. A dry lunar mantle reservoir for young mare basalts of Chang’e-5[J]. Nature,2021,600(7887):49-53.doi:10.1038/s41586-021-04107-9 [44] HONNIBALL C I,LUCEY P G,LI S,et al. Molecular water detected on the sunlit Moon by SOFIA[J]. Nature Astronomy,2021,5(2):121-127.doi:10.1038/s41550-020-01222-x [45] LI S,LUCEY P G,MILLIKEN R E,et al. Direct evidence of surface exposed water ice in the lunar polar regions[J]. Proceedings of the National Academy of Sciences,2018,115(36):8907-8912.doi:10.1073/pnas.1802345115 [46] 郑永春,王世杰,刘春茹,等. 月球水冰探测进展[J]. 地学前缘,2004,11(2):573-578.doi:10.3321/j.issn:1005-2321.2004.02.028ZHENG Y C,WANG S J,LIU C R,et al. Review on exploration of water ice on the Moon[J]. Earth Science Frontiers,2004,11(2):573-578.doi:10.3321/j.issn:1005-2321.2004.02.028 [47] 杜宇,盛丽艳,张熇,等. 月球水冰赋存形态分析及原位探测展望[J]. 航天器环境工程,2019,36(6):607-614.doi:10.12126/see.2019.06.012DU Y,SHENG L Y,ZHANG H,et al. Analysis of the occurrence mode of water ice on the moon and the prospect of in-situ lunar exploration[J]. Spacecraft Environment Engineering,2019,36(6):607-614.doi:10.12126/see.2019.06.012 [48] 何成旦,李亚胜,温智,等. 月表水冰探测与赋存形态研究进展[J]. 真空与低温,2021,27(6):589-600.doi:10.3969/j.issn.1006-7086.2021.06.011HE C D,LI Y S,WEN Z,et al. Research progress of lunar surface water ice detection and occurrence form[J]. Vacuum and Cryogenics,2021,27(6):589-600.doi:10.3969/j.issn.1006-7086.2021.06.011 [49] STACY N J S,CAMPBELL D B,FORD P G. Arecibo radar mapping of the lunar poles:a search for ice deposits[J]. Science,1997,276(5318):1527-1530.doi:10.1126/science.276.5318.1527 [50] SPUDIS P D,BUSSEY D B,BALOGA S M,et al. Initial results for the north pole of the Moon from Mini-SAR,Chandrayaan-1 mission[J]. Geophysical Research Letters,2010,37(6):L06204. [51] NOZETTE S,SPUDIS P,BUSSEY B. The lunar reconnaissance orbiter miniature radio frequency(Mini-RF)technology demonstration[J]. Space Science Reviews,2010,150:285-302.doi:10.1007/s11214-009-9607-5 [52] THOMPSON T W,USTINOV E A,HEGGY E. Modeling radar scattering from icy lunar regoliths at 13 cm and 4 cm wavelengths[J]. Journal of Geophysical Research,2011,116(E1):E01006. [53] NEISH C D,BUSSEY D B J,SPUDIS P,et al. The nature of lunar volatiles as revealed by Mini-RF observations of the LCROSS impact site[J]. Journal of Geophysical Research,2011,116(E1):E01005. [54] FA W Z,CAI Y Z. Circular polarization ratio characteristics of impact craters from Mini-RF observations and implications for ice detection at the polar regions of the Moon:lunar CPR properties for ice detection[J]. Journal of Geophysical Research:Planets,2013,118(8):1582-1608. [55] MITROFANOV I G,SANIN A B,BOYNTON W V,et al. Hydrogen mapping of the lunar south pole using the LRO neutron detector experiment LEND[J]. Science,2010,330(6003):483-486.doi:10.1126/science.1185696 [56] SUNSHINE J M,FARNHAM T L,FEAGA L M,et al. Temporal and spatial variability of lunar hydration as observed by the deep impact spacecraft[J]. Science,2009,326(5952):565-568.doi:10.1126/science.1179788 [57] CLARK R N. Detection of adsorbed water and hydroxyl on the Moon[J]. Science,2009,326(5952):562-564.doi:10.1126/science.1178105 [58] LUCEY P G. Potential for pre-biotic chemistry at the poles of the Moon[C]//Instruments, Methods, and Missions for Astrobiology III. San Diego, CA: SPIE, 2000. [59] LI S,MILLIKEN R E. Water on the surface of the Moon as seen by the Moon mineralogy mapper:distribution,abundance,and origins[J]. Science Advances,2017,3(9):e1701471.doi:10.1126/sciadv.1701471 [60] DEUTSCH A N,HEAD J W,NEUMANN G A. Analyzing the ages of south polar craters on the Moon:implications for the sources and evolution of surface water ice[J]. Icarus,2020,336:113455.doi:10.1016/j.icarus.2019.113455 [61] CRIDER D H,VONDRAK R R. The solar wind as a possible source of lunar polar hydrogen deposits[J]. Journal of Geophysical Research:Planets,2000,105(E11):26773-26782.doi:10.1029/2000JE001277 [62] SCHORGHOFER N,LUCEY P,WILLIAMS J-P. Theoretical time variability of mobile water on the Moon and its geographic pattern[J]. Icarus,2017,298:111-116.doi:10.1016/j.icarus.2017.01.029 [63] FISHER E A,LUCEY P G,LEMELIN M,et al. Evidence for surface water ice in the lunar polar regions using reflectance measurements from the lunar orbiter laser altimeter and temperature measurements from the Diviner lunar radiometer experiment[J]. Icarus,2017,292:74-85.doi:10.1016/j.icarus.2017.03.023 [64] CRIDER D H. Space weathering effects on lunar cold trap deposits[J]. Journal of Geophysical Research,2003,108(E7):5079.doi:10.1029/2002JE002030 [65] RUBANENKO L,AHARONSON O. Stability of ice on the Moon with rough topography[J]. Icarus,2017,296:99-109.doi:10.1016/j.icarus.2017.05.028 [66] KLEINHENZ J, MCADAM A, COLAPRETE A, et al. Lunar water ISRU measurement study (LWIMS): establishing a measurement plan for identification and characterization of a water reserve[R]. [S. l]: NASA, 2020. [67] SAKATANI N,OGAWA K,IIJIMA Y,et al. Experimental study for thermal conductivity structure of lunar surface regolith:effect of compressional stress[J]. Icarus,2012,221(2):1180-1182.doi:10.1016/j.icarus.2012.08.037 [68] SAKATANI N,OGAWA K,ARAKAWA M,et al. Thermal conductivity of lunar regolith simulant JSC-1A under vacuum[J]. Icarus,2018,309:13-24.doi:10.1016/j.icarus.2018.02.027 [69] HORAI K. The effect of interstitial gaseous pressure on the thermal conductivity of a simulated Apollo 12 lunar soil sample[J]. Physics of the Earth and Planetary Interiors,1981,27(1):60-71.doi:10.1016/0031-9201(81)90087-X [70] WECHSLER A E,GLASER P E. Pressure effects on postulated lunar materials[J]. Icarus,1965,4(4):335-352.doi:10.1016/0019-1035(65)90038-2 [71] OLHOEFT G R,FRISILLO A L,STRANGWAY D W. Electrical properties of lunar soil sample 15301,38[J]. Journal of Geophysical Research,1974,79(11):1599-1604.doi:10.1029/JB079i011p01599 [72] CHUNG D H,WESTPHAL W B,OLHOEFT G R. Dielectric properties of Apollo 14 lunar samples[J]. Geochimica et Cosmochimica Acta,1972(3):3161-3172. [73] ZHENG Y,WANG S,OUYANG Z,et al. CAS-1 lunar soil simulant[J]. Advances in Space Research,2009,43(3):448-454.doi:10.1016/j.asr.2008.07.006 [74] BATTLER M M,SPRAY J G. The Shawmere anorthosite and OB-1 as lunar highland regolith simulants[J]. Planetary and Space Science,2009,57(14-15):2128-2131.doi:10.1016/j.pss.2009.09.003 [75] TAYLOR L A,PIETERS C M,BRITT D. Evaluations of lunar regolith simulants[J]. Planetary and Space Science,2016,126:1-7.doi:10.1016/j.pss.2016.04.005 [76] TAYLOR L. Status of lunar regolith simulants and demand for Apollo lunar samples[R]. [S. l]: Simulant Working Group of the Lunar Exploration Analysis Group and Curation and Analysis Planning Team for Extraterrestrial Materials, 2010. [77] LUCEY P. Understanding the lunar surface and space-moon interactions[J]. Reviews in Mineralogy and Geochemistry,2006,60(1):83-219.doi:10.2138/rmg.2006.60.2 [78] NEEDHAM D H,KRING D A. Lunar volcanism produced a transient atmosphere around the ancient Moon[J]. Earth and Planetary Science Letters,2017,478:175-178.doi:10.1016/j.jpgl.2017.09.002 [79] JACQUETAB E,ROBERTB F. Water transport in protoplanetary disks and the hydrogen isotopic composition of chondrites[J]. Icarus,2013,223(2):722-732.doi:10.1016/j.icarus.2013.01.022 [80] LÉCUYERA C,GILLETA P,ROBERTB F. The hydrogen isotope composition of seawater and the global water cycle[J]. Chemical Geology,1998,145(3-4):249-261.doi:10.1016/S0009-2541(97)00146-0