基于多因子综合评估的月球探测软着陆区域及最佳巡航路线分析

选择合适的软着陆区域及规划合理的巡航路线是月球探测的基础工作。以位于月球背面南极—艾肯（South Pole-Aitken,SPA）盆地内的冯·卡门（Von Kármán）撞击坑作为研究区域,综合使用多因子分析评估了月球探测的着陆区域和巡航路线。评价体系主要包括能表征着陆安全性的撞击坑的密度、撞击坑的影响区域、整个区域的平整情况、部分区域的平整情况等因子和体现科学探索意义的区域垂直结构、岩石属性和（FeO+TiO₂）含量等因子,其中科学探索的评估分析是在安全可行性的基础上进行的。结果表明：在多因子叠加分析的基础上可选择出A、B及C 3个着陆区,并通过科学研究因子分析出路线2及路线3为合适的巡航路线。本研究为月球探测器着陆和巡航路线的规划提供了科学依据,为后续的月球探测工作提供了技术支持。     

Analysis of the brightness temperature features of the lunar surface using 37 GHz channel data from the Chang'E-2 microwave radiometer

Compared with other remote observations, brightness temperatures (T_B) derived from microwave emission measurements provide a unique means to characterize the physical properties of the lunar surface. Using Chang’E-2 microwave radiometer data, we produced 12 global T_B images of the lunar surface during a diurnal cycle with different local times separated by approximately 2?h. There are two types of remarkable T_B units on the lunar surface, the “hot regions” occurring during the lunar day in the lunar Maria regions and the “microwave cold spots” occurring during the nighttime typically related to young craters. Compared with their surroundings, the hot regions are much warmer during the lunar day and slightly colder at night, while the microwave cold spots are much colder during the lunar night and slightly warmer in the daytime. Moreover, the T_B heating and cooling rates of these two units are larger than others at the same average latitude where they are located during the lunar day, especially after sunrise and before sunset. The hot regions have a good agreement with the mare regions with high TiO₂ abundance. Besides, brightness temperatures in the lunar Maria correlate closely with their TiO₂ abundance. For most microwave cold spots, they agree with the young craters, and their brightness temperature distributions have a significant negative correlation with the lunar surface nighttime temperature and rock abundance.     

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研究了Nb离子注入的γ-TiAl合金在1123K和1173K空气中的高温循环氧化行为,用配有能谱仪的扫描电子显微镜对氧化层的形貌、显微结构进行了分析,用俄歇谱仪分析了注入元素和氧化层中各元素的分布.结果表明:Nb离子注入可以提高γ-TiAl合金的抗循环氧化性能.提高其抗氧化性能的主要原因归结于Nb离子在TiO₂中的掺杂作用.高价Nb的掺杂,降低了TiO₂的缺陷浓度,使TiO₂的生长受到抑制,在氧化初期形成了Al₂O₃保护层,从而推迟了氧化层的剥落时间.但Nb离子注入的γ-TiAl合金不具有长期的抗循环氧化性能.     

激光快速熔凝Al2O3/YAG共晶陶瓷的制备与组织

采用激光快速熔凝技术制备Al₂O₃/YAG共晶自生复合陶瓷, 研究Al₂O₃/YAG共晶陶瓷在高能激光束作用下,不同扫描速率(0.01~2.0mm/s)、超高温度梯度下的凝固组织特征及其生长机制,探索激光熔凝过程控制参数与凝固组织的关系.研究结果表明:激光熔凝Al₂O₃/YAG共晶陶瓷由无规则连续分布的Al₂O₃相和YAG相两相组成,没有晶界和其他相,Al₂O₃相的体积分数为(45.0±2.0)%,两相耦合生长,交错分布,是典型的快速凝固层片状非规则共晶组织;共晶层间距细密, 并随激光扫描速度的增大而减小,扫描速度为0.02mm/s 时,共晶间距约为1~2μm,扫描速度为2.0mm/s时,共晶间距仅为0.5μm左右;综合热分析表明,Al₂O₃/YAG共晶熔点为2096K,与相图吻合.     

Titanium estimates of the central peaks of lunar craters: Implications for sub-surface lithology of moon

Central peaks of 24 lunar craters, having mafic rocks, were studied to estimate their average titanium content and infer the nature of the subsurface lithologies. Titanium contents were derived from Clementine UV–Vis data (415, 750 nm) following the approach of Lucey et al. [Lucey, P.G., Blewett, D.T. and Jolliff, B.L., Lunar iron and titanium abundance algorithms based on final processing of Clementine ultraviolet–visible images, J. Geophys. Res.106 (E8), 20297–20,305, 2000]. _TiO2${\mathrm{TiO}}_2$ content exceeding 1 wt% suggests presence of mantle derived mafic sub-surface rock types (plutonic/volcanic) within the central peaks. Even though, the algorithm used for deriving titanium content is susceptible to variation in topography and sun angle, especially at higher latitudes, careful selection and analyses of data for regions within the central peaks revealed compositional heterogeneities. The results indicate a preponderance of mafic lithologies with low _TiO2${\mathrm{TiO}}_2$ content (<1 wt%) in the central peaks of lunar craters populating the equatorial region. Average titanium content of central peaks can serve as a useful tracer for distinguishing mantle derived mafic subsurface lithologies from those formed during global magma ocean episode.     

Libration point orbits for lunar global positioning systems

With the development of lunar exploration, a lunar global positioning system (LGPS) is demanded for both on-ground and in-flight lunar exploration missions. The traditional configuration of constellation requires at least eighteen satellites to cover the whole lunar surface continuously. In this paper, the configurations of the libration point orbits (LPOs) constellations are investigated. By using the constellations on the Earth–Moon _L1$L_1$ and _L2$L_2$ LPOs, the basic functions of the LGPS can be realized by using eight to fourteen satellites. First, the LPO and the combinations of LPOs, which can be used in the constellations of the LGPS, are investigated. The criteria and procedures of the configuration design are introduced. Second, the configurations of LPOs constellations are investigated in the Earth–Moon circular-restricted three-body problem (CR3BP). The size of the LPOs and the distribution of the satellites on these LPOs are determined by using an exhaustive algorithm and a global optimization method, respectively. The key performance parameters of these constellations are computed. Third, the constellations with good performance in the CR3BP are redesigned in the more accurate Earth–Moon based Sun-perturbed bicircular four-body problem (B4BP). Moreover, in order to avoid the ground coverage problem caused by the perturbation of the Sun, some modifications are implemented, and the configuration of the no blind area LGPS in the B4BP is obtained.     

铝合金阳极化膜上铈转化膜沉积的电化学研究

阳极氧化膜在含1g/L CeCl₃和2.7 g/L H₂O₂的水溶液中阴极电解可以在其表面沉积富铈转化膜.用循环伏安、φ-t和j-t曲线等电化学测试方法对转化膜成膜反应进行了研究,以期获得对成膜机理的深入了解和证实根据其它工作提出的成膜机理.研究结果表明铈转化膜的生成包括阳极氧化膜的化学溶解和4价铈化合物的电化学还原两个过程;在阴极电位达到析氢电位之前,这两个过程主要是由H₂O₂在阴极的电还原改变了阴极表面附近溶液的局部pH值引起的,而O₂的还原通常不能引起这两个过程的发生.      

Sulfur “concrete” for lunar applications – Sublimation concerns

Melting sulfur and mixing it with an aggregate to form “concrete” is commercially well established and constitutes a material that is particularly well-suited for use in corrosive environments. Discovery of the mineral troilite (FeS) on the moon poses the question of extracting the sulfur for use as a lunar construction material. This would be an attractive alternative to conventional concrete as it does not require water. However, the viability of sulfur concrete in a lunar environment, which is characterized by lack of an atmosphere and extreme temperatures, is not well understood. Here it is assumed that the lunar ore can be mined, refined, and the raw sulfur melded with appropriate lunar regolith to form, for example, bricks. This study evaluates pure sulfur and two sets of small sulfur concrete samples that have been prepared using JSC-1 lunar stimulant and SiO₂ powder as aggregate additions. Each set was subjected to extended periods in a vacuum environment to evaluate sublimation issues. Results from these experiments are presented and discussed within the context of the lunar environment.     

Calculation of fast neutron removal cross sections for different lunar soils

The interaction of galactic cosmic rays (GCRs) and solar energetic particles (SEPs) with the lunar surface produces secondary radiations as neutrons. The study of the production and attenuation of these neutrons in the lunar soil is very important to estimate the annual ambient dose equivalent on the lunar surface and for lunar nuclear spectroscopy. Also, understanding the attenuation of fast neutrons in lunar soils can help in measuring of the lunar neutron density profile and to measure the neutron flux on the lunar surface. In this paper, the attenuation of fast neutrons in different lunar soils is investigated. The macroscopic effective removal cross section (_ΣR)$({\mathrm{\Sigma }}_R)$ of fast neutrons was theoretically calculated from the mass removal cross-section values (_ΣR/ρ)$({\mathrm{\Sigma }}_R/\rho )$ for various elements in soils. The obtained values of (_ΣR)$({\mathrm{\Sigma }}_R)$ were discussed according to the density. The results show that the attenuation of fast neutrons is more important in the landing sites of Apollo 12 and Luna 16 than the other landing sites of Apollo and Luna missions.     

三层月壤模型的多通道微波辐射模拟与月壤厚度的反演

由月球表面数字高程试验性地构造了整个月球表面月壤厚度的分布.根据Clementine探月卫星的紫外-可见光光学数据,计算了整个月球表面月壤中FeO+TiO2含量分布,给出了整个月球表面月壤介电常数分布.由月球表层温度的观测结果以及月壤的导热特性,给出了月尘层与月壤层温度随纬度分布的经验公式.在这些条件的基础上,建立了月尘、月壤、月岩三层微波热辐射模型.由起伏逸散定理,模拟计算了该月球模型多通道辐射亮度温度.然后,以此辐射亮度温度模拟加随机噪声为理论观测值,按三层模型提出了月壤层厚度反演方法.由于高频通道穿透深度小,由高频通道的辐射亮度温度按照两层月尘-月壤微波热辐射模型反演月尘层与月壤层的物理温度,再由穿透深度较大的低频通道辐射亮度温度反演月壤层厚度.对于反演的相对误差也进行了讨论.      

钛合金的离子束改性

钛合金是航空航天工业常用的结构材料,它具有重量轻、强度高、抗腐蚀强等优良性能,但耐磨性较差.为提高其耐磨性,对TC4、TA7航材试件,采用溅射方法在其表面镀上钛膜,并用(N^＋＋N^＋₂)混合离子束进行动态反冲注入及单元素C^＋离子束注入两种方法,进行表面改性.精密摩擦、磨损试验及显微硬度测量结果,试件表面的滑动摩擦系数降低了64%~77%;磨损率减少了22%~48%;显微硬度提高0.3~1.4倍.证明离子注入有效地改善了合金表层的摩擦、磨损性能.对注入样品进行X射线光电子能谱(XPS)分析,发现注入后的钛合金表层,生成了大量的TiO₂,并析出TiN,TiC等金属化合物,这是降低摩擦系数,提高耐磨性的主要因素.添加C^＋离子注入的试件,其力学性能并无进一步改善,原因有待分析.     

等离子喷涂纳米TiO2涂层及其光催化性能

原始喷涂粉末经过喷雾干燥法造粒,采用等离子喷涂工艺在普通载玻片上制备了纳米TiO₂涂层,并对涂层在300℃,400℃,500℃进行热处理.采用X射线衍射(XRD)方法对TiO₂涂层进行了相结构分析;用扫描电子显微镜(SEM)、透射电子显微镜(TEM)观察涂层的微观形貌;用压汞方法测量涂层的孔隙率.结果表明,喷涂后锐钛矿型TiO₂含量大约在30%~50%,粒径10~30nm,孔隙率小于6%,热处理后涂层更致密,孔隙率降低.喷涂电流为400A且未经过热处理的TiO₂涂层具有最佳光催化效果.     

基于“嫦娥2号”CELMS数据的冯·卡门撞击坑微波辐射特性

冯·卡门（Von Kármán）撞击坑位于月球背面的SPA盆地西北部,切穿了浅层月壳,具有异常的矿物成分分布。基于微波辐射计数据的月壤微波辐射特性分析,对月球热演化和岩浆演化研究具有重要的参考价值。本研究基于“嫦娥2号”卫星微波辐射计数据,采用时角分析、双线性插值方法,生成了研究区域的亮温（T_B）图和亮温差（dT_B）图像;结合Arcgis软件,叠加地质图,并结合成分、地形图,研究了Von Kármán撞击坑微波辐射特性。研究结果表明：研究区北部出现高T_B异常,初步判定为下垫面温度较高;研究区南部出现与钛铁矿（FeO+TiO₂）含量分布相对应的亮温表现;结合研究区的微波辐射特性,重新进行了冯·卡门撞击坑地质解译;根据冯·卡门撞击坑的亮温表现,建议北部为着陆区重点选择区,其次为南部和西部。     

Experimental investigation on deformation behavior of TJ-1 lunar soil simulant subjected to principal stress rotation

The knowledge of mechanical properties of lunar soil is of fundamental importance for the coming exploration of the Moon. This paper aims to investigate the fundamental deformation behavior of lunar soil and the effects of the intermediate principal stress coefficient, deviatoric stress ratio, and mean stress during the principal stress rotation. First, an improved technique was proposed to generate homogeneous samples based on the Multi-layer Undercompaction Method. Second, three series of tests on TJ-1 lunar soil simulant under the principal stress rotation were performed with a hollow cylinder apparatus at Tongji University, China. In each series of tests, only one value of the three variables mentioned above was changed while the others were kept constant. The test results demonstrate that the rotation of principal stress can result in significant plastic deformation, volumetric strain, and non-coaxiality (non-coincidence of the increment direction of principal plastic strain with the principal stress direction) of TJ-1 lunar soil simulant. In addition, it is found that the intermediate principal stress coefficient, deviatoric stress ratio, and mean stress have different influences on the four strain components, i.e. _εz,_εr,_εθ${\epsilon }_z\text{,}{\epsilon }_{\text{r}}\text{,}{\epsilon }_{\theta }$ and _γzθ${\gamma }_{z\theta }$, volumetric strain, and non-coaxiality during the principal stress rotation. The influence of deviatoric stress ratio is relatively stronger than the others. Therefore, the influence of principal stress rotation on the deformation behavior of lunar soil should be taken into account carefully in the design and construction of facilities on the lunar surface in the future.     

Long-wavelength lunar gravity field recovery from simulated orbit and inter-satellite tracking data

As has been demonstrated recently, inter-satellite Ka-band tracking data collected by the GRAIL (Gravity Recovery And Interior Laboratory) spacecraft have the potential to improve the resolution and accuracy of the lunar gravity field by several orders of magnitude compared to previous models. By means of a series of simulation studies, here we investigate the contribution of inter-satellite ranging for the recovery of the Moon’s gravitational features; the evaluation of results is made against findings from ground-based Doppler tracking. For this purpose we make use of classical dynamic orbit determination, supported by the analysis of satellite-to-satellite tracking observations. This study sheds particularly light on the influence of the angular distance between the two satellites, solar radiation modeling and the co-estimation of the lunar Love number k₂. The quality of the obtained results is assessed by gravity field power spectra, gravity anomalies and precision orbit determination. We expect our simulation results to be supportive for the processing of real GRAIL data.     

月球粒子辐射环境探测现状

月球表面没有磁场的保护,粒子辐射是人类在月球活动的重要风险要素。概述了月球的辐射环境以及辐射来源,并介绍了月球探测的现状,特别提及了近年来几个较为典型的月球辐射探测实例及其探测结果;介绍了我国“嫦娥4号”上搭载的月表中子与辐射剂量探测仪（Lunar Lander Neutron&Dosimetry,LND）的科学目标及其技术指标。LND的科学目标主要包括：载人登月辐射剂量的测量、月球南极艾特肯盆地水含量的测量、艾特肯盆地FeO含量的测量,以及为日球层科学的研究提供依据。     

Using high-energy proton fluence to improve risk prediction for consequences of solar particle events

The potential for exposure to large solar particle events (SPEs) with high energy levels is a major concern during interplanetary transfer and extra-vehicular activities (EVAs) on the lunar and Mars surface. Previously, we have used data from the last 5 solar cycles to estimate percentiles of dose to a typical blood-forming organ (BFO) for a hypothetical astronaut in a nominally shielded spacecraft during a 120-d lunar mission. As part of this process, we made use of complete energy spectra for 34 large historical SPEs to calculate what the BFO mGy-Eq dose would have been in the above lunar scenario for each SPE. From these calculated doses, we then developed a prediction model for BFO dose based solely on an assumed value of integrated fluence above 30 MeV (Φ₃₀) for an otherwise unspecified future SPE. In this study, we reasoned that since BFO dose is determined more by protons with higher energies than by those with lower energies, more accurate BFO dose prediction models could be developed using integrated fluence above 60 (Φ₆₀) and above 100 MeV (Φ₁₀₀) as predictors instead of Φ₃₀. However to calculate the unconditional probability of a BFO dose exceeding a pre-specified limit (“BFO dose risk”), one must also take into account the distribution of the predictor (Φ_30,Φ₆₀, or Φ₁₀₀), as estimated from historical SPEs. But Φ₆₀ and Φ₁₀₀ have more variability, and less available historical information on which to estimate their distributions over many SPE occurrences, than does Φ₃₀. Therefore, when estimating BFO dose risk there is a tradeoff between increased BFO dose prediction at a given energy threshold and decreased accuracy of models for describing the distribution of that threshold over future SPEs as the threshold increases. Even when taking the second of these two factors into account, we still arrived at the conclusion that overall prediction improves as the energy level threshold increases from 30 to 60 to 100 MeV. These results can be applied to the development of approaches to improve radiation protection of astronauts and the optimization of mission planning for future space missions.     

Theoretical modelling of X-ray fluorescence signals for different lunar compositions and dependence on solar activity

We present a forward modelling technique for calculating the surface X-ray spectra for a variety of lunar terrains. Our calculations considered variations in solar fluxes from solar quiescent condition to large flare activity (M1 flare), and expected elemental concentrations in the target, as well as yield, instrumental, and viewing geometry parameters for X-ray induced fluorescence from the lunar surface. Additionally, we present estimates of anticipated XRF signals from prominent K_α lines observable by a collimated 14 cm² X-ray detector from a 100 km lunar orbit with ∼20 km spatial resolution. Our results show that Mg, Al and Si characteristic K_α lines can be observed for all solar conditions. The Ca K_α lines line can be differentiated from a fixed background during more energetic solar conditions such as C1 and M1 flares, whereas Ti and Fe lines are identifiable only during C1 and M1 solar flare conditions for Apollo 12 site composition. Both the K_α X-ray intensity ratios of Mg/Si and Al/Si correlate well with concentration ratios of Mg/Si and Al/Si, respectively, for B1 and M1 solar conditions. The K_α X-ray intensity ratios of Fe/Si and Ca/Si correlates with concentration ratios of Fe/Si and Ca/Si, respectively, for M1 solar condition. In principle, the modelling technique outlined here can be used to determine absolute elemental abundances (Mg, Al, Si, Ca, Ti and Fe) from X-ray spectra measured during recent and future lunar missions.     

Upwards migration phenomenon on molten lunar regolith: New challenges and prospects for ISRU

As part of our research on the feasibility of producing commodities from lunar regolith by thermal-driven processes with minimal terrestrial precursors we need to characterize, reproduce, and understand thermophysical properties of the molten regolith still unforeseen under the lunar vacuum conditions at a scalable sample size. Two unanticipated phenomena, apparently caused by lunar melt’s surface tension under vacuum, have been revealed in our research work, vacuum void formation and upwards migration. In this paper we present our findings and thinkable explanation on the upwards migration phenomenon experimentally observed and consistently replicated as JSC-1A lunar regolith simulant melted at high vacuum. Upwards migration of molten lunar regolith will make future lunar ISRU’s melting processes both challenging as molten bulk material would migrate upwards along the container’s walls, and also promising on new opportunities for alternative ISRU’s sustainable processes as regolith’s upwards migration takes place in uniformed thin-film pattern. Among the potential ISRU’s processes that might use controlled thermal thin-film-based migration without the necessity of terrestrial precursors are production of feedstock for 3D printing, fractional separation of regolith’s component’s (O₂, metals, and alloys) via pyrolysis, film coating, purification of valuables solid crystals including silicon, and fabrication of key elements for microfluidic, and MEMS devices. Thermal upwards migration phenomenon on JSC-1A’s melt is formulated and explained by the authors as due to thermal Marangoni effect (also known as thermo-capillarity) in which temperature gradients within the melt’s bulk and along the crucible’s wall yield the surface tension large enough to supersede the gravitational force and yield the experimentally observed upwards thin-film migration. As far as the authors know, upwards thermal migration of molten JSC-1A (or other lunar simulant regolith) under vacuum has not been reported in the literature. A thermal mathematical model accounting for thermal Marangoni effect on molten JSC-1A agrees with what experimentally was observed, the formation of the meniscus on the melt-wall surface interface along with an incipient upwards migration in thin-film pattern along the crucible wall that, according to the model, experiences large temperature gradient, an important factor to trigger the thermal Marangoni effect along with the fact that surface tension of the molten lunar regolith material is temperature dependent.     

O2 evolution and cyclic electron flow around photosystem I in long-term ground batch culture of Euglena gracilis

Based on the purpose of better exploring the function of green producers in the closed aquatic biological life support system, the condition of dynamic O₂ evolution and performance of cyclic electron flow around photosystem I (CEF-PSI) in long-term ground batch culture of Euglena gracilis were studied, the relationship between linear electron flow (LEF) and CEF-PSI was revealed, the function of CEF-PSI was investigated. Excellent consistency in O₂ evolution pattern was observed in cultures grown in both closed and open containers, O₂ evolution was strictly suppressed in phase 1, but the rate of it increased significantly in phase 2. CEF-PSI was proposed to be active during the whole course of cultivation, even in the declining phase 3, it still operated at the extent of 47–55%. It is suggested that the relationship between LEF and CEF-PSI is not only competition but also reciprocity. CEF-PSI was proposed to contribute to the considerable growth in phase 1; it was also suggested to play an important protective role against photosystem II (PSII) photoinhibition at the greatly enhanced level (approximately 80–95%) on the 2nd day. Our results in this research suggest that E. gracilis had very particular photosynthetic characteristics, the strict O₂ evolution suppression in the initial culture phase might be a special light acclimation behavior, and CEF-PSI could be an important mechanism involved in this kind of adaptation to the changeable light environment.