月尘静电迁移研究进展

月尘的静电悬浮和迁移是Apollo时期留下的最有争议的问题之一. 其既是研 究月球表面物质演化历史的重要线索, 也是探月工程必须考虑的重要因素. 月尘在月表环境下易因电子附着、光电效应、二次电子发射等过程带电, 并 在月球全球性静电场作用下发生迁移运动. 但目前对月尘静电迁移过程的认 识还不全面, 其主要原因在于对月尘静电特性的了解不够准确, 对静电迁移 过程的地面模拟不够充分以及对月球尘埃环境的探测较为缺乏. 未来需进一 步开展模拟月尘的研制, 月尘静电特性的分析, 静电迁移过程模拟以及尘埃 环境的探测等工作.      

发动机羽流作用下的实时月尘运动仿真

月尘运动是月球探测器软着陆过程中不可或缺的重要环节,针对发动机羽流作用下月尘运动真实感不强和月尘颗粒运动模型过于简单的问题,提出了一种逼真的实时月尘运动仿真方法.通过计算流体动力学(CFD, Computational Fluid Dynamics)和二次谢别德插值(Quadratic Shepard)方法,分析和计算单个月尘颗粒的运动学模型,得到一定初始条件下粒子运动的二维轨迹曲线;通过分析粒子的数量、初始位置、初始速度、生命周期等参数对粒子运动学的影响和变化规律,抽象出月尘系统的粒子集;建立基于月尘粒子集的月尘运动模型.实验结果显示:该运动模型逼真的模拟了发动机羽流作用下月尘腾起、飞溅、弥漫、消散等运动过程,视觉真实感和实时性能良好,对研究真空环境中的月尘运动及月球软着陆等相关领域具有一定的参考意义.目前该方法已应用于北航虚拟现实国家重点实验室月球软着陆仿真系统.     

悬浮月尘的遮挡模型

探月活动中,月表的尘埃会对太阳翼等光电器件的工作效率造成严重影响.基于附着月尘的遮挡模型,从立体空间的角度分析了悬浮月尘对工作器件的遮挡,提出了悬浮月尘的单粒度遮挡模型,利用月尘的平均粒度可计算在指定立体空间内,定量月尘造成的遮挡量;引入月尘的粒度分布函数,提出了悬浮月尘的多粒度遮挡模型,能够计算已知粒度分布函数的月尘在指定立体空间内造成的遮挡量;通过设计悬浮月尘遮挡的仿真实验,分别利用3种不同粒度大小的月尘进行实验,实验数据与悬浮月尘的单粒度、多粒度遮挡模型的理论计算值都较好吻合,实验结果证实了悬浮月尘遮挡模型的正确性与可靠性.      

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.      

模拟月壤可行驶性的离散元数值分析

基于模拟月壤扫描电镜显微照片,建立土颗粒的几何模型,提出不规则形状颗粒群系统的生成策略,构建模拟月壤颗粒间接触的简化本构模型,并利用量纲分析法和双轴压缩试验离散元模拟,建立土宏观力学特性与细观模型参数的关系,结合模拟月壤的三轴压缩试验数据确定离散元模型参数.在月球重力环境下,对轮-土交互作用进行离散元模拟,推导土壤推力的细观表达式,定性分析不同滑转率时土颗粒的动态行为,定量分析模拟月壤的可行驶性.研究结果表明,土壤推力随滑转率的提高而增大;当车轮以高滑转率行驶时,土壤推力相对行驶时间存在瞬态和稳态2个阶段,并且瞬态值高于稳态值.     

月球探测车转向系统动力学建模与分析

月球探测车在月球表面松软土壤上的转向动力学特性比较复杂。文章在已有的车辆地面力学成果的基础上 ,研究了探测车在松软的月球表面土壤上的转向动力学问题。给出了六轮月球探测车的四轮转向运动学计算公式 ,推导了探测车在松软土壤上的四轮转向动力学模型 ,提出了合理的简化方法 ,并对稳态特性进行了相应的分析。所得到的结果为探测车转向系统设计及控制算法研究提供了依据     

月球着陆器软着陆冲击仿真

为提高分析月球着陆器软着陆有效载荷着陆冲击响应的准确性,提出一种基于瞬态动力学的着陆器有效载荷软着陆冲击响应分析方法.根据着陆器全机结构柔性和月壤柔性对有效载荷着陆冲击响应的影响,参照某型着陆器,于MSC.PATRAN环境中建立着陆器全机柔性体模型及月壤柔性体模型,运用瞬态动力学仿真软件MSC.DYTRAN对着陆器软着陆有效载荷着陆冲击响应特性进行了仿真研究.仿真结果与试验结果具有一定的一致性.研究结果表明:使用该方法分析着陆器软着陆有效载荷的着陆冲击响应是准确有效的,能够比较逼真地模拟月球着陆器实际着陆工况.     

基于刚柔耦合模型的月球着陆器动力学分析

基于刚柔耦合多体动力学理论,提出了一种基于三维实体造型、有限元分析与多体动力学分析的刚柔耦合动力学仿真分析方法;利用该方法建立了月球着陆器着陆动力学模型,分别在地球重力环境和月球重力环境(1/6地球重力环境)下,对某典型着陆工况下的着陆动力学进行了仿真分析,得到了着陆器着陆的缓冲性能分析结果,包括主支柱最大缓冲行程、左右辅助支柱最大缓冲行程、最大质心加速度响应;将仿真结果与试验结果相比较,验证了着陆器动力学模型的正确性以及仿真分析方法的有效性,为今后的着陆器缓冲试验提供了动力学模型和仿真分析方法.从能量角度对月球着陆器的着陆过程进行分析,弥补了缓冲试验难以进行能量分析的不足.     

地面观测研究彗星尘埃的一种新方法

本文根据尘埃吸收系数Q_v的不同模型(由实验和观测建立的模型)求解了不同性质的尘埃的辐射平衡方程.得到了性质不同,颗粒大小不同,日心距不同的尘埃的温度.如果我们把邻近两个波长的观测到的强度比值所确定的色温度当作尘埃的真实温度,那么我们就能够通过近红外的地面观测来研究尘埃的性质(而不要远红外的空间观测).      

月球天梯力学特性研究

月球天梯的构型对其力学特性和质量特性起决定性作用,直接关系到天梯建造材料的选取。目前对月球天梯的研究集中在组合横截面积构型上,未对其他构型天梯的特性展开深入研究。针对这一问题,文章进行了不同构型月球天梯的力学特性研究。建立了月球天梯动力学模型,分别将天梯缆绳线密度和应力作为常值,推导了等横截面积和变横截面积两种新构型月球天梯的动力学方程和质量特性方程,进行了不同构型天梯关键特性参数的计算和对比分析。研究结果表明,变横截面积天梯可将最大应力设计为任意恒定值,降低了对材料极限应力的要求,其总质量小于等横截面积和组合横截面积天梯,为最优构型方案。     

Plasma electron temperature variability in lunar surface potential and in electric field under average solar wind conditions

The Moon is immersed in plasma environment. The most interesting challenge of the lunar plasma– field environment is that it is alternatively dominated by the extended but variable outer atmosphere of the Earth – the magnetosphere – and by the extended but highly variable solar atmosphere – the solar wind. Understanding the plasma environment and its interaction with the lunar surface will be beneficial to both manned and robotic surface exploration activities and to scientific investigations. Presented is a preliminary map of variations of lunar surface electric potential over the day side and night side using probe equations and a discussion on dust dynamics in this E-field structure using the data from Electron Reflectometer in Lunar Prospector spacecraft during 1998–1999. On the day side, potential is around 5 V and on the night side it reaches up to −82 V. On the night side region, only highly energetic electrons can overcome this large negative potential. The variation at electron temperature (T_e) strongly reflects in the surface potential. The potential reaches to a value of −82 V for T_e = 58 eV. Surface charging causes the electrostatic transport of charged dust grains. Dust grain size of 0.1 μm shows a levitation height of 4.92 m on lunar day side, 748 m on terminator region and 3.7 km on the night side. The radius of maximum sized grain to be lofted, R_max, peaks at the terminator region (R_max = 0.83 μm). At the transition region dust levitation is almost absent. This region is most suited for exploration activities as the region is free from hazards caused by lunar dust.     

Electrostatic particle collection in vacuum

Lunar grains accumulate charges due to solar-based ionizing radiations, and the repelling action of like-charged particles causes the levitation of lunar dust. The lunar dust deposit on sensitive and costly surfaces of investigative equipment is a serious concern in lunar explorations. Inspired by electrostatic precipitators (ESPs), the Electrostatic Lunar Dust Collector (ELDC) was proposed for collecting already charged lunar dust particles to prevent the lunar dust threat. As the conditions for terrestrial counterparts are not valid in the lunar environment, equations developed for terrestrial devices yield incorrect predictions in lunar application. Hence, a mathematical model was developed for the ELDC operating in vacuum to determine its collection efficiency. The ratios of electrical energy over potential energy, kinetic energy over potential energy and the ratio of ELDC dimensions were identified to be the key dimensionless parameters. Sensitivity analyses of the relevant parameters showed that depending on ELDC orientation, smaller particles would be collected more easily at vertical orientation, whereas larger particles were easier to collect in a horizontal ELDC configuration. In the worst case scenario, the electrostatic field needed to be 10 times stronger in the vertical mode in order to adequately collect larger particles. The collection efficiency was very sensitive to surface potential of lunar dust and it reached the maximum when surface potential was between 30 and 120 V.     

Formation of Saturn's spokes

The scattering properties of the spokes in Saturn's rings suggest that they consist of micron-sized dust particles. We suggest that these grains are elevated above the ring plane by electrostatic charging. We show that electrostatic levitation requires a sufficiently large plasma density near the rings. If the plasma density near the rings exceeds a few 10² cm^?3 levitation may occur at significant rates in the strong electric fields which exist in the wall-sheaths at the ring. Once the dust particles are elevated they drift relative to the plasma (except at synchronous orbit). This relative motion constitutes a current which causes a polarization electric field if the plasma is azimuthally inhomogeneous. The dense plasma will drift radially in response to this electric field and cause levitation of more dust particles as it moves along. It leaves a radially aligned trail of elevated dust particles—the spokes. One way of producing dense plasma is by meteor impact on the rings. We discuss the mechanisms of ring charging, electrostatic levitation and the currents in the plasma-dust mixture. We show that for reasonable conditions spokes of more than 10,000 km radial length can be formed in less than five minutes. We also show that under the same conditions the electrostatic levitation model predicts a dust grain population which peaks at a size of 0.6 microns and can reach optical depths of 0.1.     

Interactions of solar wind plasma with dust grains: Effects of strong plasma anisotropy

In this paper we re-examined the fundamental physics of charging of a dust particle in the moon environment by tenuous anisotropic solar wind plasma. The majority of work on dusty (complex) plasmas is largely concerns with laboratory plasmas, in which charging process of dust grains is very fast, thus making practical the working concept of dynamically equilibrium floating potential and grain charge. However, solar wind plasma parameters are considerably different at the moon orbit, and we found the characteristic charging time of lunar dust grains to be considerably longer, ranging from 3 to 4.6 min for micron size particles, and up to 7.6 h for 10-nm grains, depending on the value of plasma streaming velocity. These findings make it clear that the transient stage of charging process is important in the moon environment, and equilibrium floating potential and grain charge could be considered as long time asymptotic values. For this reason we re-formulated the moon dust charging process as an inherently time-dependent problem and derived the time-dependent charging equation for the grain potential for general case of anisotropic solar wind plasma. Using the results of our kinetics analysis we found that the distribution of charge density over grain surface submerged into solar wind plasma is highly anisotropic, thus making the OML model, which is based on the assumption of isotropic distribution of surface charge density, not applicable to the grain charging problem by the solar wind plasma.     

极月轨道上太阳电池阵外热流规律分析

准确的月球表面温度分布模型对于开展月球探测具有重要意义. 目前有关月球表面温 度模型还缺乏对完整月球表面温度分布的计算方法研究. 本文建立了一套计算完整月球表面温度的方法, 其中月球阳面温度采用Racca模型直接计算得到; 对于月球阴面, 将其沿纬度方向划分为若干区域, 每个区域的地表土壤采用一维非稳态热传导模型, 根据嫦娥三号着陆器太阳电池阵在轨环月阶段的温度数据, 修正得到月球表面土壤导热系数、密度及比热容, 通过数值计算求解一维非稳态热传导方程, 得出任意时刻月球阴面表面温度随时间的变化. 嫦娥三号着陆器太阳电池阵环月阶段热分析结果与在轨温度符合较好, 初步说明本文建立的完整月球表面温度计算方法正确可行. 基于本文方法计算得到整个月球表面温度分布, 进一步研究了极月轨道太阳电池阵外热流变化规律.      

Effects of electrostatic forces on the vertical structure of planetary rings

We have calculated the vertical structure of planetary dust rings as it results from a balance between an electrostatic force on the dust grains and the vertical component of the gravitational force from the central planet. The electrostatic force results from the charging of the dust grains by the ambient plasma and a large scale electric field due to a shielding electric field and the resulting vertical dust distribution are strongly dependent on dust size, dust and plasma density, plasma temperature and plasma ion type. The dust density distribution has a different dependence on these parameters in tenuous and in dense dust rings. We solve the relevant equations numerically and also by linearization in the limiting cases of tenuous or dense rings. Our results indicate that the effects treated in this paper may be important in both Jupiter's and Saturn's rings.     

月球着陆器着陆过程动力学分析

以哈尔滨工业大学宇航空间机构及控制研究中心研制的四腿桁架式月球着陆器样机为研究对象,通过简化模型,导出了着陆器着陆过程中各个着陆脚和着陆器质心在惯性坐标系中的位置坐标方程,以此位置坐标方程为依据得到了着陆器准静态稳定性条件.通过分析着陆器与月面着陆时瞬态动力学行为,得到了着陆器在此瞬态的各动力学参数的计算公式,以此为依据,并离散时间变量,给出了可以程序化实现整个动态着陆过程动力学模拟的计算过程,为进一步研究着陆过程动力学行为奠定了基础.