Metallic and Oxidized Aluminum Debris Impacting the Trailing Edge of the Long Duration Exposure Facility (LDEF)

A total of 87 microcraters >30 m in diameter that were found in gold substrates exposed on the trailing edge of the non-spinning Long Duration Exposure Facility (LDEF) yielded analyzable projectile residues in their interiors. Using qualitative SEM-EDS analysis methods, some 60 of these craters were formed by natural cosmic-dust particles, while 27 residues (31%) were assigned to orbital debris (Hörz et al., 1993). The far majority of the orbital-debris impacts, 24 (89%) of the 27 events, contained only aluminum in their X-ray spectra. The present study evaluates these aluminum-rich residues in detail and employs a windowless X-ray detector, which permits for the analysis of low-Z elements and specifically of oxygen. This makes it possible to discriminate between oxidized (Al₂O₃) and metallic (Al) projectiles from dramatically different sources, the former produced during solid-fuel rocket firings, the latter resulting from explosively or collisionally disrupted spacecraft.Of the 24 craters analyzed with the windowless detector, 13 (54%) contained Al₂O₃ and 11 (46%) yielded structurally disintegrated Al metal. The oxidized residues preferentially occur in the smaller craters, all <60 m in diameter. Corresponding particles on LDEF's trailing edge are <35 m in diameter. Some 70% of this particle population is composed of Al₂O₃. Although solid-fuel rocket exhaust products are typically <5 m in size, they tend to coagulate into crusts at the rocket nozzle to be shed occasionally as relatively large, aggregate particles. Structurally disintegrated, metallic fragments compose one-third of all particles <35 m, but they dominate all particles >35 m, and thus all craters >60 m. These findings clearly establish that solid-rocket exhaust particles, as well as explosively or collisionally produced debris, exist in low-inclination, high-eccentricity orbits in sufficient quantities that they must be accounted for in models describing the present and future orbital-debris population at typical Shuttle and Space Station altitudes.     

The MAGO experiment for dust environment monitoring on the Martian surface

Among the main directions identified for future Martian exploration, the study of the properties of dust dispersed in the atmosphere, its cycle and the impact on climate are considered of primary relevance. Dust storms, dust devils and the dust “cycle” have been identified and studied by past remote and in situ experiments, but little quantitative information is available on these processes, so far. The airborne dust contributes to the determination of the dynamic and thermodynamic evolution of the atmosphere, including the large-scale circulation processes and its impact on the climate of Mars. Moreover, aeolian erosion, redistribution of dust on the surface and weathering processes are mostly known only qualitatively. In order to improve our knowledge of the airborne dust evolution and other atmospheric processes, it is mandatory to measure the amount, mass-size distribution and dynamical properties of solid particles in the Martian atmosphere as a function of time. In this context, there is clearly a need for the implementation of experiments dedicated to study directly atmospheric dust. The Martian atmospheric grain observer (MAGO) experiment is aimed at providing direct quantitative measurements of mass and size distributions of dust particles, a goal that has never been fully achieved so far. The instrument design combines three types of sensors to monitor in situ the dust mass flux (micro balance system, MBS) and single grain properties (grain detection system, GDS + impact sensor, IS). Technical solutions and science capabilities are discussed in this paper.     

航空发动机砂尘吸入物静电监测仿真实验

提出了航空发动机砂尘吸入物静电监测的仿真实验方法,实验以软件ANSYS电磁场分析模块建立有限元模型为基础,模拟不同粒径、荷质比、运动速度及质量浓度情况下砂尘吸入物的静电感应信号,并分别从时域与频域对感应电荷与电压信号进行分析,研究砂尘吸入物的粒径及其他宏观参数与静电监测信号之间的关系,建立用以表征砂尘颗粒粒径大小的特征指标。基于IDMS(进气监测系统)感应电压信号功率谱密度分布建立了特征向量,并以其曼哈顿距离与欧氏距离作为特征指标表征砂尘颗粒粒径大小。经仿真实验验证:特征指标与砂尘粒径呈正相关,且不受砂尘吸入物运动速度及荷质比变化的影响,但受砂尘吸入物质量浓度影响。进一步研究将利用质量浓度对特征指标进行修正,并开展验证实验。      

火星尘埃对太阳电池阵的影响与电帘除尘研究

火星表面大量尘埃在太阳电池阵表面的累积将会导致其输出功率下降,甚至使太阳电池阵功能失效。近年来,电帘除尘方法被认为是在火星着陆任务中进行尘埃防护最有效的手段之一。本文开展了火星尘埃累积对三结砷化镓太阳电池性能影响的实验研究,得到了火星尘埃累积量与太阳电池电压、电流和相对输出功率数值模型;通过除尘技术分析,确定电帘除尘装置构型;依据制备得到的除尘电帘,对不同火星尘埃累积下电帘的除尘效率进行了研究,为火星着陆太阳电池阵遥测数据分析和开发自适应除尘太阳电池阵提供有力的技术支持。     

月球受光面上月尘静电浮扬特性分析

基于单粒子轨道理论及空间尘埃等离子体充电方程,建立了月球受光面上尘埃微粒的静态荷电模型.基于光电子能量Maxiwellian分布假设,确定了月面垂直空间电场强度和光电子鞘层内带电粒子密度的函数表达式.利用牛顿运动定律和静电场力表达式,构建了月球受光面上尘埃微粒的静电浮扬动力学模型,并进行月尘静态浮扬特性的数值计算.研究结果显示:太阳高度角与颗粒粒径是控制月尘静电浮扬发生及动力学特性的两个基本参量;月尘静电浮扬发生在月球的黎明和黄昏;随着粒径的减少,月尘颗粒的最大浮扬高度不断增加.     

火星太阳电池翼除尘方法综述

“萤火一号”火星探测器即将发射升空,标志着我国火星探测计划实施的开始。然而,火星尘埃在范德华力和静电力的作用下积聚在太阳电池翼的表面,使其转换效率下降,影响火星探测器的寿命。因此,开展火星太阳电池翼除尘技术的研究是非常有意义的。文章主要介绍了火星太阳电池翼的除尘方法,特别是目前最受关注的电帘除尘方法,并对其基本结构、除尘原理、除尘效率和透光性做了详细的描述,对开展火星太阳电池翼除尘技术的研究具有一定的参考作用。     

管道相连泄爆容器中粉尘爆炸的实验研究

采用管道相连容器进行了工业规模的粉尘爆炸实验,目的是研究粮食粉尘在管道相连的加工和输送工业设备中发生粉尘爆炸时火焰和爆炸压力的传播过程及粉尘的Kst值对爆炸的影响。实验装置为一个气力输送系统,由两个不同体积的容器通过管道连接构成。采用粮食工业上具有代表性的两类粉尘进行了粉尘爆炸测试,爆炸从一个容器中通过管道传播到另一个容器中并引发了随后的二次爆炸,测试了不同位置的火焰和压力信号。实验结果表明：即使在起爆容器采取了泄爆措施,管道中没有粉尘喷入的情况下,粉尘爆炸火焰也可沿管道传播达30m并引发二次爆炸;随着粉尘爆炸指数的增大,初始爆炸的猛烈程度增强,火焰传播速度加快,二次爆炸的猛烈程度也随之增强。     

一种微米级粒子的静电发射加速装置

为了研究空间微小碎片碰撞对航天器的影响,国内外研制了各种类型的微小碎片加速器。文章简要介绍了一种很有前景的静电式微小碎片加速器及其关键部件的工作原理、结构特点及适用范围等。     

高压涡轮尾切凹槽叶尖冷却换热特性

为研究尾切凹槽状涡轮叶片叶尖的表面换热,通过瞬态风洞实验得到无冷却和带除尘孔两种情况下叶尖表面传热系数,并将其与数值模拟结果进行对比,实验结果的不确定度小于5%。分析叶尖间隙流场情况,无冷却时,由于腔底的空腔涡和凸肩壁的分离泡,高表面传热系数集中在压吸力侧凸肩和腔底前缘处;腔底后半段沿压力侧存在条状低表面传热系数分布。有除尘孔冷却时,冷却气体分为高低能两股流体,高能流体随泄漏流流出,造成吸力侧凸肩存在多段高表面传热系数集中分布;低能流体紧贴凹槽压力侧向后流动,对应位置冷却效率可达0.4以上。      

异型(三叶形)截面碳化硅纤维的异形度控制

以聚碳硅烷（ＰＣＳ）为原料,采用熔融纺丝制备三叶形ＰＣＳ纤维后,经不熔化和烧成制得异形度为０．６５～０．８５的三叶形碳化硅纤维。研究了纺丝温度、压力、收丝速度等对纤维异形度的影响,并对预氧化和烧成工艺进行了研究,研究表明,氏的纺丝温度、适当主的纺丝压力和较低的转率有效于提高纤维的异形度,聚碳硅烷原丝经预氧化和烧结后,纤维异形度基本保持不变。