砂尘环境试验风洞压力特性及控制策略

砂尘环境试验风洞的压力调节方式不同于常规回流式风洞,为了研究风洞中压力变化的动态特性,进行合理分析与简化后,应用集总参数法建立起风洞压力控制点、试验段及加砂段压力变化的动态特性模型,给出了相应的控制策略.通过仿真试验得出不同扰动因素对压力分布的影响规律,在此基础上对砂尘环境试验风洞的压力控制系统进行了仿真研究.能够有效优化风洞结构、提高承压能力及确定各部件控制精度.     

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.     

KM6载人航天器空间环境试验设备

KM6载人航天器空间环境试验设备是中国最大的一台空间环境模拟试验设备 ,是国际上五大典型空间环境试验设备之一。已建成的有 9个分系统 ,模拟室由三舱组合 ,主模拟室直径 1 2 m、高 2 2 .4m,极限真空度 4.5× 1 0 - 6Pa、热沉温度 1 0 0 K,主要性能达到国际先进水平。文章对其技术指标、系统组成、功能、特点进行了介绍 ,并给出了试验结果 ;对研制过程中的重要技术问题进行了分析     

大流量气-气喷嘴响应面法优化设计

为研究以气氢和气氧为推进剂的同轴双剪切喷嘴设计参数对推进剂燃烧位置的影响,利用正交表指导喷嘴设计,并对燃烧室流场进行数值模拟.结果表明:在单喷嘴流量相当于航天飞机主动发动机单喷嘴流量8倍的工况下,同轴双剪切喷嘴能实现高的燃烧效率;极差和方差分析显示氢/氧的速度比是对推进剂的燃烧位置影响最大的设计参数,而中心氢流量比例和氧喷嘴的壁厚对燃烧位置的影响不显著.通过构造基于正交多项式的响应面,获得同轴双剪切气-气喷嘴的优化组合参数.     

人造卫星的力学环境试验

<正> 一、引言地面环境试验是保证人造卫星可靠性的重要一环.为了进行环境试验,不仅要化大量人力物力建立各种试验设备,而且试验费用也是相当可观的.据国外估计,一个卫星型号的试验费用约占整个研制费用的1/5～1/3(美国军方估计约30-50%,NASA哥达德空间飞行中心估计为5-15%,欧洲空间局估计约1/3).人造卫星在发射过程中所经受的噪声、振     

稳态等离子体推进器羽流场数值模拟

采用二维轴对称模型,使用粒子网格法(PIC)和直接模拟蒙特卡洛法(DSMC)相结合的方法,对稳态等离子体推进器(SPT)羽流场进行了数值模拟.采用DSMC方法中的随机取样频率法(RSF)求解粒子碰撞过程,并对比了不同的分配电荷方式、电子运动模型及SPT出口条件时的羽流场.将不同条件计算得到的羽流场中距SPT出口0.1?m,0.5?m及1.0?m处的离子电流密度和电荷密度与实验结果进行了对比,得出在采用面积权重法分配电荷、等熵模型描述电子运动和用实验值设定发动机出口参数时对SPT羽流场数值模拟的电流密度和轴向附近的电荷密度结果与实验结果符合程度较好的结论.     

2 AU以内的“渐进型”太阳高能粒子事件模拟

太阳高能粒子（Solar Energetic Particle,SEP）事件是影响地球空间以及深空辐射环境的主要因素之一。“渐进型”太阳高能粒子事件中的高能粒子主要来自于日冕物质抛射（Coronal Mass Ejection,CME）所驱动的激波扩散加速（Diffusive Shock Acceleration,DSA）过程。CME驱动的激波在行星际的传播过程中,其结构不断演化,进而影响到高能粒子的加速过程。本文利用二维太阳高能粒子加速和传播模型,对发生于2014年4月18日的太阳高能粒子事件实例进行了数值模拟。模型考察了黄道面上2 AU的距离以内包含地球所在位置的4个不同点,分别计算了每个点上高能粒子的通量。数值模拟的结果表明：黄道面内不同位置的观察点,与激波波前的磁力线连接不同,从而导致观察点处高能粒子的通量有着显著的差异。该模型的计算结果可以为深空探测计划开展辐射环境研究提供必要的输入。     

失重条件下低温推进剂排放计算

针对CZ-3A系列运载火箭三子级低温贮箱内剩余推进剂排放问题,分别对排放过程中液氢和液氧低温推进剂沿2种不同排放管的流动进行了一维数值计算和分析.计算中认为在排放时沿管路压强降低,从而引起液体推进剂气化,并在管路的某个位置出现气固两相或者全部气化,在计算中,根据不同位置时推进剂的不同状态,分别采用液相、气液两相、气固两相及气相的物理数学模型和控制方程.计算得出了排放的出口参数及排放性能,认为液氢从通道1排放比较好,液氧从通道2排放比较好.为进一步进行排放研究提供了依据.      

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.      

航空发动机喷嘴结焦积碳的性质

针对航空燃料燃烧时会在航空发动机喷嘴处产生大量结焦积碳,影响航空飞行器的飞行安全和使用寿命这一问题,研究了某型航空发动机喷嘴零部件上结焦积碳的生成情况.采用扫描电镜(SEM,Scanning Electron Microscope)、透射电镜(TEM,Transmission Electron Microscopy)、能谱仪(EDS,Energy Disperse Spectroscopy)以及X射线衍射技术(XRD,X-ray Diffraction)对结焦积碳的微观形态和性质进行了分析.结果表明:喷嘴零部件上生成的结焦积碳主要有两种形态:一种是丝状焦,另一种是颗粒状焦.其中,丝状焦只出现在零部件表面较光滑的位置,包括短纤维丝状焦和不定形丝状焦,是由金属催化作用所形成的;其形成与喷嘴零部件的结构、材质及表面粗糙度有关.颗粒状焦则主要集中在活塞表面,包括颗粒团聚状焦和颗粒分散状焦,是由催化作用与燃料热裂解共同作用所形成的.      

火星表面风沙物理过程及沙尘暴的起动风速

通过建立风吹动地表沙粒运动的模型并根据大气湍流边界层风速廓线规律,计算了火星上沙尘暴的起动风速和沙尘暴发生时空中悬浮沙尘粒径的大小,并对沙粒从地面跳起进入气流的方式进行了验证.发现当大气为中性层结时,火星沙尘暴的起动需要离地面2m高处的风速达到28.7m·s-1.在起动临界风速下,地表沙粒需要滚动一个粒径的距离才能跳起,沙尘暴发生后,火星大气中悬浮沙尘的粒径小于30μm.      

A synchrotron-based facility for the in-situ location,chemical and mineralogical characterization of ∼10 μm particles captured in aerogel

NASA’s Stardust mission collected dust from the coma of Comet Wild-2 on January 2nd, 2004, by direct capture into aerogel cells that flew through the dust coma at ∼6 km/s. Stardust collected several hundred comet particles >10 μm in size. These comet samples were delivered to Earth on January 15th, 2006. We developed a facility at the National Synchrotron Light Source at Brookhaven National Laboratory (Upton, NY, USA) for the in-situ characterization of ∼10 μm particles collected in aerogel. These analytical instruments allow us to perform extensive chemical, mineralogical, and size-frequency characterization of particles captured in aerogel. These analyses are conducted without any invasive extraction, minimizing the possibility of contamination or particle loss during preparation. This facility was used to determine the chemical composition, the oxidation state, the mineralogy and to provide an indication of the grain size of the Wild-2 particles before they were removed from the aerogel. This information provides a catalog of particle types, allowing a more reasoned allocation of the particles to subsequent investigators based on a relatively detailed knowledge of the chemical composition and mineralogy of each particle. These measurements allowed a comparison of the chemical and mineralogical properties of the Wild-2 particles with other types of extraterrestrial materials, including interplanetary dust particles and meteorites. The success of in-situ analysis for Wild 2 particles demonstrates that synchrotron-based facilities will be important for the analysis of particles collected in aerogel on future earth-orbiting satellites and spacecraft.     

Size distributions of circumplanetary dust

Dust rings have been observed around each of the giant planets and may also exist around Mars. The particles comprising these rings have short lifetimes due to a number of processes including exospheric and plasma drag, Poynting-Robertson drag, sputtering, collision with other circumplanetary particles, and the Lorentz force for charged grains. The supply of dust is maintained by collisions between macroscopic ring particles and bombardment of moons and ring particles by interplanetary impactors. All of the processes that act to remove or alter the circumplanetary dust grains are functions of particle size, so the initial size distribution of the grains released from an impact onto a moon or ring particle is modified. The size distribution of the impact ejecta can be described by a power-law of the form n(r)dr ∝r^−qdr where n(r)dr is the number of particles in the size range [r,r + dr] and q is the power-law index. For hypervelocity impact excavation, q ≈ 3.5. Drag acts more efficiently on smaller grains resulting in a reduction in q of 1. Other dynamical processes can lead to particle-size dependent collision rates with other circumplanetary objects. These processes can lead to local steepening of the size distribution (increase in q) and to truncation of the dust size distribution to a narrow range of sizes.     

A fine mist of very small comet dust particles

A comet nucleus considered as an aggregate of interstellar dust would produce a mist of very finely divided (radius ～ 0.01 μm) particles of carbon and metal oxides accompanying the larger dust grains. These small particles which are very abundant in the interstellar dust size spectrum would provide substantial physical effects because of their large surface area. They may show up strongly in particle detectors on the Halley probes. A strong basis for serious consideration of these particles comes from the other evidence that interstellar dust grains are the building blocks of comets; e.g. (1) the explanation of the “missing” carbon in comets; (2) The S₂ molecule detection which suggests that the comet solid ice materials have been previously subjected to ultraviolet radiation (as are interstellar grains) before aggregation into the comet; (3) the predicted dust to gas ratio.     

On the evolution of dust in the solar vicinity.

The analysis of interplanetary dust shows that the majority of particles in out-of-ecliptic regions comes from comets and also that near solar dust, in the ecliptic regions, results most probably largely from comets. The intense radiation flux in the solar vicinity is expected to cause strong modifications in the material composition and surface structure of interplanetary dust particles and hence the analysis of near solar dust provides interesting insights into the evolution of meteoritic, especially cometary materials. Because of the lack of in-situ measurements our present knowledge concerning these processes derives from remote sensing, i.e. observations of the solar F-corona. In particular these are observations of albedo, polarization and colour temperature given in terms of average particle properties. For example the analysis of near infra-red F-corona data points to the existence of a strong component of irregularly structured silicate particles, most probably of cometary origin. The data may indicate a subsequent sublimation of different particles or different constituents of the particles. Here we compare particle properties derived from F-corona observations with model calculations of single particle properties and discuss perspectives of future analysis of cometary dust in the interplanetary cloud.     

The Halley dust model

The properties of dust ejecta from Comet Halley are studied on the basis of (a) evidence from the comet's past apparitions and (b) analogy with recent, physically similar comets. Specifically discussed are the light curve and spectrum, discrete phenomena in the head, the physical properties of the nucleus (size, albedo, rotation, surface temperature, and morphology), and an interaction between the nucleus and dust atmosphere. Also reviewed are constraints on the size and mass distributions of dust particles, information on submicron-size and submillimeter-size grains from the comet's dust tail and antitail, and the apparent existence of more than one particle type. Similarities between the jet patterns of Halley and the parent comet of the Perseid meteor stream are depicted, and effects of the surface heterogeneity (discrete active regions) on the dust flow are assessed. Current dust models for Halley are summarized and the existence of short-term variations in the dust content in the comet's atmosphere is suggested.     

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.      

水介质中降落球形塑料颗粒与静止气泡的 黏附行为

为了揭示球形塑料颗粒在气泡表面的黏附行为及机理,采用高速摄影仪对自由降落的球形塑料颗粒与固定在水槽中静止气泡的黏附过程进行拍摄,利用图像处理方法提取颗粒黏附过程运动特性曲线及碰撞角与运动时间的关系,研究颗粒碰撞位置、颗粒和气泡直径对黏附行为的影响。实验结果表明:颗粒的黏附主要分为碰撞黏附和滑动黏附,气泡表面的滑动壁面假设与实验值的吻合度较高。此外,通过对实验数据的统计发现,随着碰撞角的增大,感应时间明显增长,但是颗粒陷入气泡表面的时间基本维持在10 ms,颗粒陷入气泡的深度受气泡和颗粒尺寸的共同影响,约占气泡与颗粒直径之和的2%。