On the effect of considering more realistic particle shape and mass parameters in MMOD risk assessments

One of the primary mission risks tracked in the development of all spacecraft is that due to micro-meteoroids and orbital debris (MMOD). Both types of particles, especially those larger than 0.1 mm in diameter, contain sufficient kinetic energy due to their combined mass and velocities to cause serious damage to crew members and spacecraft. The process used to assess MMOD risk consists of three elements: environment, damage prediction, and damage tolerance. Orbital debris risk assessments for the Orion vehicle, as well as the Shuttle, Space Station and other satellites use ballistic limit equations (BLEs) that have been developed using high speed impact test data and results from numerical simulations that have used spherical projectiles. However, spheres are not expected to be a common shape for orbital debris; rather, orbital debris fragments might be better represented by other regular or irregular solids. In this paper we examine the general construction of NASA’s current orbital debris (OD) model, explore the potential variations in orbital debris mass and shape that are possible when using particle characteristic length to define particle size (instead of assuming spherical particles), and, considering specifically the Orion vehicle, perform an orbital debris risk sensitivity study taking into account variations in particle mass and shape as noted above. While the results of the work performed for this study are preliminary, they do show that continuing to use aluminum spheres in spacecraft risk assessments could result in an over-design of its MMOD protection systems. In such a case, the spacecraft could be heavier than needed, could cost more than needed, and could cost more to put into orbit than needed. The results obtained in this study also show the need to incorporate effects of mass and shape in mission risk assessment prior to first flight of any spacecraft as well as the need to continue to develop/refine BLEs so that they more accurately reflect the shape and material density variations inherent to the actual debris environment.     

SRAM FPGA电离辐射效应试验研究

针对SRAM FPGA空间应用日益增多,以100万门SRAM FPGA为样品,进行了单粒子效应和电离总剂量效应辐照试验。单粒子试验结果是:试验用粒子最小LET为1.66 MeV·cm2/mg,出现SEU（单粒子翻转）;LET为4.17 MeV·cm2/mg,出现SEFI（单粒子功能中断）,通过重新配置,样品功能恢复正常;LET在1.66～64.8 MeV?cm2/mg范围内,未出现SEL（单粒子锁定）;试验发现,随SEU数量的累积,样品功耗电流会随之增加,对样品进行重新配置,电流恢复正常。电离总剂量辐照试验结果是:辐照总剂量75 krad(Si)时,2只样品功能正常,功耗电流未见明显变化。辐照到87 krad(Si)时,样品出现功能失效。试验表明SRAM FPGA属于SEU敏感的器件,且存在SEFI。SEU和SEFI会破坏器件功能,导致系统故障。空间应用SRAM FPGA必须进行抗单粒子加固设计,推荐的加固方法是三模冗余（TMR）配合定时重新配置（Scrubbing）。关键部位如控制系统慎用SRAM FPGA。     

NASA空间环境及效应(SEE)计划进展

文章介绍了NASA在1993年提出的空间环境及效应(下称SEE)计划,其目的是明确空间环境的定义,为设计、研制能适应严酷空间环境效应的航天器系统并使其正常运行提供技术支持.该计划包括认识空间环境、飞行试验和地面试验技术的优化、更新空间环境及其效应的预测模型、保存信息并将之纳入航天器的设计流程等方面.文章描述了SEE计划目前已取得的成就和未来的打算.     

卫星姿控发动机喷管羽流撞击效应试验

在高超声速低密度风洞中试验研究了卫星姿控发动机喷管羽流对平板模型的撞击效应,包括气动力和气动热效应。试验气体为加热的氮气。对两个卫星姿态控制发动机喷管的十种实验状态进行了测量。测出了平行于喷管轴线的平板模型上的压力分布和温度变化及处于喷管上方后流区的挡板的温度变化,给出了平板模型上的气动力和气动热分布规律,并判断是否形成后流区。测量结果表明,试验结果可靠,具有工程应用价值,能为姿控发动机在卫星上的布局提供参考。     

风洞模拟建筑物对大气污染物扩散影响的若干问题讨论

通过相似性分析,得到了大气污染建筑物影响风洞试验应满足的基本相似条件.由一个实例研究了利用常规风洞模拟装置和测试仪器进行大气污染建筑物影响风洞试验在技术上的可行性.结果显示:由于模拟装置和仪器条件的限制,在大多数风洞试验中存在大气边界层不完全模拟和仪器响应过慢等问题,但通过合理模拟来流的主要湍流特征和改进采样方法,可以在风洞中较真实地模拟建筑物对大气扩散的影响.     

含边界和损伤因素的纺织复合材料细观胞元模型

纺织复合材料的细观力学分析通常以胞元模型为基础,胞元边界条件的合理施加是获得精确分析结果的关键之一。本文以平面机织复合材料为例,讨论了细观胞元的选取和周期边界条件的施加方法,在此基础上建立了二维细观有限元模型,通过与全厚度模型分析结果的比较,研究了周期胞元模型的合理性,特别是边界效应和局部损伤等非周期因素对分析结果的影响,给出了这些因素下胞元边界条件的处理方法。     

地球同步轨道高压太阳电池阵充放电效应研究

地球同步轨道(GEO)高压太阳电池阵表面静电放电(ESD)引起二次放电可能导致太阳电池阵永久性短路损坏。文章主要针对GEO高压太阳电池阵充放电效应问题,重点分析了高压太阳电池阵表面ESD和二次放电产生的物理过程,并利用负高压偏置方法开展了GEO高压太阳电池阵表面ESD和二次放电地面模拟试验。试验验证了反转电位梯度电场是导致GEO高压太阳电池阵表面产生ESD的触发因素之一,同时得到了GaAs高压太阳电池阵样品表面产生ESD和二次放电的电压阈值。     

Investigation on the interface damage in drilling low-stiffness CFRP/Ti stacks

Carbon fiber reinforced plastic and titanium alloy (CFRP/Ti) stacks have been widely used as aerospace structures because of their excellent combination of physical properties. Interface damage caused by interface gaps, significantly different from that of metal/metal stacks, is a common problem in the through-hole drilling of CFRP/Ti stacks with low stiffness. In this study, a force–deformation coupling model was developed to further examine the formation mechanism and the control method of interface damage. Firstly, the coupling model was built considering the interaction between the thrust force and the deformation. To solve this model, a numerical method was proposed in which specific cutting coefficients were calibrated using only the thrust force of rigid stacks. Secondly, drilling experiments were performed with different feed rates and bending stiffness. Experimental results indicate that interface damage mainly includes interlayer chips and surface damage of CFRP layers. The surface damage, which is irreparable, is caused by the rotary extension of metal chips along the interlayer gap. Thirdly, variations of the interface gap were calculated with the coupling model that had been verified by measured thrust forces. The damage area was found to have a linear dependence relation with the interlayer gap. However, in conditions of large gap sizes, the interface damage areas increased with the interlayer gap at high feed rates, while decreasing slightly at low feed rates. This phenomenon was satisfactorily explained by the presented model. Finally, a method was proposed to determine the appropriate pressure exceeding which no interlayer damage will occur. Additional drilling experiments proved the method effective. This study leads to further understanding of the forming mechanism of interlayer damage and of selecting appropriate parameters in drilling low-stiffness composite/metal stacks.     

PROBLEMS OF WINDBLAST

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Latitude and solar-cycle dependence of radial IMF intensity

I describe a simple procedure for extrapolating the observed solar magnetic field into the heliosphere, which averages the asymptotic fields computed using the standard source surface and current sheet models. The resultant field is characterized by strong latitudinal gradients (maintained by volume currents outside the source surface) and by abrupt reversals in direction at the current sheets. The model yields good agreement with the observed long-term variation of the radial IMF component in the ecliptic, and is used to predict the variation of |B _r | along the latitudinal trajectory of Ulysses during 1990–1994. As found in earlier studies, the magnitude ofB _r at any latitude is determined largely by the strength and relative orientation of the Sun's dipole moment.