开发月球

1969年7月到1972年12月，美国实施“阿波罗”计划，先后6次将12人送上月球，在月面上进行了大量的科学探测活动。自那时以来，人们一直在希望重返月球，逐步在月面上建立起驻入基地，然后进一步开发月球。     

月球主要构造特征：嫦娥一号月球影像初步研究

月球在31亿年前已基本停止地质活动,从而保留了其形成初期的信息．这些信息对于认识月球、地球乃至太阳系的形成演化具有重要意义．在已有研究成果的基础上,结合嫦娥一号探月卫星CCD影像数据,从月海穹窿、撞击坑、月岭、断裂、月坑链、月溪及月谷等方面介绍了月球主要构造形式的地质特征、形貌特征及遥感影像特征,对其成因以及所隐含的地质意义进行了分析．结果表明,嫦娥一号CCD影像信息丰富,影像清晰,利用其CCD影像数据进一步研究月球的构造现象是可行的．     

月震特征及与地震的对比

月球内部结构是月球研究的热点问题，月震是研究月球内部结构的最佳手段之一.对月震数据及震源参数进行了再分析，在分析已有研究结果的基础上，对各类月震的信号特征、震源分布以及震源机制进行讨论，并将其与地震进行对比.研究发现，月震与地震有很多明显差异:月震信号持续时间较长，且深源月震与热月震具有波形匹配特征；探测到的月震多为深源月震，主要分布于月球正面的北东向和南西向；深源月震和热月震的发震时间都具有周期性，深源月震的周期性主要由地球对月球的潮汐引力以及太阳对月球轨道的扰动造成，且其发震位置具有丛集性，即在相同或相近位置重复发生，而热月震的周期性主要由于月球昼夜温度变化造成.      

一片冰心在玉壶“月球勘探者”证实月球存在水冰

一片冰心在玉壶“月球勘探者”证实月球存在水冰□□１９９８年３月５日，美国航宇局的刘易斯研究中心，向新闻界公布了“月球勘探者”探测器获得的第一批月球探测结果，证实了月球上确实存在水冰，并初步测算出月面上水的总储量可能在１１×１０６ｔ～３．３×１０８ｔ之...     

清镇陨石（EH3）中陨硫钙石的REE微量元素及成因意义

本文运用INAA分析了14个清镇陨石中陨硫钙石单矿物颗粒的难熔元素(La、Ce、Sm、Eu、Yb、Lu、Ca、Sc、Hf和Th),挥发性元素(Na、Cr、Zn、Se、Br等)和亲铁元素(Fe、Ni、Co、Ir、Au、As)含量。结果表明陨硫钙石高度富集难熔亲石元素,是顽火辉石陨石中REE的主要载体,携带了约80％的全岩REE总量。相对于HREE,LREE有更大的富集程度,而且早期凝聚的颗粒较晚期凝聚的颗粒更富集REE,同时陨硫钙石富集挥发性元素Se、Br等。清镇陨硫钙石的微量元素特征揭示了它来自于太阳星云的高温凝聚特征和成因。     

月球表面水冰的探测和意义

综述了月表水冰的发现，探测技术，水资源的存在形式，分布，资源量，月表水的运移和利用前景，已有的探测表明，月球上的水资源主要分布在两极的永久阴影区内，储量约为66亿吨。月表水冰主要分布于两极永久阴影区中的原因，是月球上的水可以通过弹道式跳跃逐步迁移到温度低的地区所致。本文认为月球上是否存在水对于人类进行月球基地的建设没有根本性的影响，而利用月球玄武岩中钛铁矿的反应来获取水，是更为简便和经济的方法。     

月球撞击坑辐射纹的形成和消失机制及可能的年代学应用

辐射纹是年轻撞击坑周缘呈辐射状分布的明亮细条纹,是月表最显著的地貌特征之一,也是月球科学领域热点研究之一.根据目前对于月球撞击坑辐射纹的形成和类型的认识,分析辐射纹消失相关的空间风化、撞击导致的物质混合等地质过程;比较不同形成年龄撞击坑辐射纹的光学成熟度(OMAT)剖面,发现溅射物逐渐成熟过程中OMAT剖面的演变过程,...     

以色列探月:就差临门一脚

<正>2019年4月14日,被以色列各界寄予厚望的"创世纪号"月球着陆器坠毁在月面上,这宣告以色列冲击"世界上第四个月球软着陆国家"的努力失败了。虽然说失败是成功之母,但最终导向成功的失败才有意义。如果详细分析"创世纪号"的飞行过程,可以发现问题还是不小的。如果SPACEIL公司和IAI公司继续按照这样的模式来研制后续月球着陆器,未必能走向成功的终     

晚期撞击事件:月球曾被撞坏?

正启动重返月球的计划,从月球背面收集样本进行研究,或许可以揭开近40亿年前若干小行星撞击月球的相关谜团。乘“阿波罗”号登月的宇航员在20世纪六七十年代曾采集回若干月球岩石样品,对这些岩石的同位素分析发现,约39亿年前(太阳系形成于约46亿年前,此时太阳系内环境已归于平静很久了),月球表面曾被若干小行星撞击过。这个神秘的事件最初被称为“月球灾     

藏匿在冯·卡门坑南部下方的月球质量瘤

月球着陆探测的候选着陆区域的质量异常分布,预示着对应区域发生过复杂的动力学演化过程,存在着异常丰富的物质组成。对月球的质量异常分布或重力场异常的探测是基于绕月卫星重力探测方法获取的,结合“嫦娥1号”月球探测获得的月球重力场异常模型与地形探测模型的数据,分析揭示存在于月球背面的质量瘤区域,研究结果表明：使用多次任务的数据首次证认了一个位于中尺度撞击区域,冯·卡门（Von Kármán）撞击坑的南半部和边缘的正下部的质量瘤,暂定编号CEFC04,冯·卡门撞击坑是该区域形成后,又一次大型撞击产生的。这类显著的被藏匿的中尺度月球质量瘤的发现,对探测研究月球的演化有重要意义。     

Next-generation electromagnetic sounding of the Moon

Electromagnetic (EM) sounding of the Moon, largely performed during the Apollo program, provided constraints on core size, mantle composition, and interior temperature. We present new analytical and numerical models that demonstrate the abilities of a next generation of EM sounding to (1) determine the electrical structure of the outermost 500 km and its lateral variability, specifically to understand the extent of upper-mantle discontinuities and the structure of the Procellarum KREEP Terrane; (2) determine the temperature and composition of the lower mantle; and (3) better constrain core size. New EM sounding need not rely on the Apollo methodology, which analyzed the magnetic transfer function between a surface station and a distantly orbiting satellite. Instead, a network of magnetometers (as few as two) can be used, or a complete sounding can be performed from a single station by measuring both electric and magnetic fields. Furthermore, in the magnetotail or lunar wake, sensors can operate from orbit, at altitudes up to the desired investigation depth. The twin-spacecraft ARTEMIS mission will test these methods and a lunar geophysical network will provide definitive results.     

固液推进技术在载人登月中的应用

通过对世界主要航天国家和地区新世纪载人登月计划的研究、美国"阿波罗"飞船登月舱动力系统的详细分析,基于固液推进技术的特点,利用遗传算法开展了固液火箭发动机替代"阿波罗"登月舱下降级和上升级液体火箭发动机方案的优化设计,并对两者在功能、质量、体积和推进剂特性上进行了对比分析.结果表明固液推进技术在载人登月以及深空探测中具有良好的应用优势和前景.     

CAS-1 lunar soil simulant

Lunar soil simulant is a geochemical reproduction of lunar regolith, and is needed for lunar science and engineering researches. This paper describes a new lunar soil simulant, CAS-1, prepared by the Chinese Academy of Sciences, to support lunar orbiter, soft-landing mission and sample return missions of China’s Lunar Exploration Program, which is scheduled for 2004–2020. Such simulants should match the samples returned from the Moon, all collected from the lunar regolith rather than outcrops. The average mineral and chemical composition of lunar soil sample returned from the Apollo 14 mission, which landed on the Fra Mauro Formation, is chosen as the model for the CAS-1 simulant. Source material for this simulant was a low-Ti basaltic scoria dated at 1600 years from the late Quaternary volcanic area in the Changbai Mountains of northeast China. The main minerals of this rock are pyroxene, olivine, and minor plagioclase, and about 20–40% modal glass. The scoria was analyzed by XRF and found to be chemically similar to Apollo 14 lunar sample 14163. It was crushed in an impact mill with a resulting median particle size 85.9 μm, similar to Apollo soils. Bulk density, shear resistance, complex permittivity, and reflectance spectra were also similar to Apollo 14 soil. We conclude that CAS-1 is an ideal lunar soil simulant for science and engineering research of future lunar exploration program.     

Identification and characterization of science-rich landing sites for lunar lander missions using integrated remote sensing observations

Despite more than 52 years of lunar exploration, a wide range of first-order scientific questions remain about the Moon’s formation, temporal evolution, and current surface and interior properties. Addressing many of these questions requires obtaining new in situ analyses or return of lunar surface or shallow subsurface samples, and hence rely on the selection of optimal landing sites. Here, we present an approach to optimize science-rich lunar landing site selection studies based on the integration of remote sensing observations. Currently available remote sensing data, as well as features of interest published in the recent literature, were integrated in a Geographic Information System. This numerical database contains geographic information about all these findings, which can be consulted and used to simultaneously display multiple features and parameters of interest. To illustrate our approach, we identified the optimal landing sites to address the two top priorities (or goals) relative to Concept 3 of the National Research Council of the National Academies (2007), namely to ‘Determine the extent and composition of the primary feldspathic crust, (ur)KREEP layer, and other products of differentiation’ and to ‘Inventory the variety, age, distribution and origin of lunar rock types’. We review site requirements and propose possible landing sites for both these goals. We identified 29 sites that best fulfill both these goals and compare them with the landing sites of planned future lunar lander missions. Finally, we detail two of these science-rich sites (Aristarchus and Theophilus craters) which are particularly accessible through their location on the nearside.     

模拟月壤研制的初步设想

模拟月壤是月球样品的地球化学复制品，作者总结世界上已有的5种模拟月壤JSC-1，MLS．1，MLS-2，MKS-1和FJS-1的研制过程、方法与基本理化性质，认为系列化模拟月壤研制对中国首次月球探测有重要意义，在此基础上，作者提出系列化模拟月壤研制的基本思路．     

月面广义资源探测及其原位利用技术构想

以载人登月场景下的月面资源精细化利用为目标,概述了月面资源探测与原位利用技术的国内外发展现状。针对未来载人登月探测任务规划以及确定预先研究目标的实际需求,提出了月面环境资源的广义分类和精细化利用思想,并以载人登月场景下的"人器机环境"系统为研究对象,细化了可在轨利用的资源、需带回地球的样本资源和人机废弃物资源等三类资源的拓扑组成。本着继承与创新兼顾、前瞻性与实用性包容的概念研究理念,重点阐述了宇航员人因主导的矿物资源勘查、月面环境条件的资源化利用、多态样本的采集、人机废弃物的循环利用等月面广义资源的探测与原位利用技术途径。     

考虑相互碰撞影响的月壤颗粒运动轨迹计算方法研究

针对登月着陆器下降过程扬起月壤颗粒的运动轨迹及空间分布问题, 提出了考虑月壤颗粒发生完全弹性碰撞和非完全弹性碰撞两种情况的月壤颗粒运动轨迹计算方法. 根据质量守恒和能量守恒定律确定月壤颗粒相互碰撞后的速度, 通过羽流场与月壤颗粒的流固耦合相互迭代计算方法, 获得被扬起的月壤颗粒在羽流场和相互碰撞共同作用下随时间的运动轨迹和空间分布. 基于美国Apollo 11登月过程实测数据, 采用数值模拟对该方法进行验证. 结果表明, 考虑月壤颗粒相互碰撞的影响后, 其运动规律出现较明显的扩散趋势. 进一步考虑月壤颗粒相互碰撞引起能量损失的影响后, 月壤颗粒的扩散趋势有所减弱, 并且扬起的高度随着恢复系数的减小而降低.      

X-ray fluorescence spectrometrywith the SELENE orbiter

X-ray fluorescence spectrometry of the Moon using a CCD-based instrument “XRS” is planned with the SELENE (Selenological and Engineering Explorer) orbiter, which will be launched in 2003. In the Apollo 15 and 16 missions, elemental mapping of Mg, Al and Si has been performed at the lunar equatorial regions for only 9% of the total surface. Much improved datasets will be obtained by using the XRS to map most of major elements, for 90% coverage of the total surface, and within 20 km spatial resolution. Key scientific objectives are (a) to measure the global average of lunar surface composition for investigation of the overall properties of lunar crust, (b) to map the rock-type distribution to study the formation and evolution of the crust and the maria, and to speculate the origin of the dichotomy, (c) to survey the chemical pattern of lava flows, or bottoms of craters or basins, for surveying the vertical structure and composition of the lunar crust and mantle. We describe the XRS instrument.     

嫦娥一号卫星CCD立体相机月表图像镶嵌

鉴于嫦娥一号CCD相机获取图像的特殊性, 选用投影的方法, 完成了Apollo12, Apollo14和Apollo15登月点区域的月表正视图像镶嵌. 在分析圆柱投影表象的基础上, 推导出了月球割35o Mercator投影公式. 首先读取单轨数据的经纬度和灰度, 进而根据四个角点的经纬度建立空图框, 并根据分辨率、长度比与月球投影理论分别在纵向和横向上进行网格划分, 实现图框的像元化. 通过单轨图像和图框的坐标匹配完成灰度镶嵌, 匹配误差控制在一个像元以内. 对重叠区域的灰度值进行平滑处理, 最终图像还原来完成月表图像的镶嵌. 该方法有普遍适用性, 可以用于其他轨道图像的镶嵌.