Whipple防护屏弹道极限参数试验

在中国空气动力研究与发展中心FD-18A超高速碰撞靶上进行了Whipple防护屏的超高速撞击试验。弹丸为LY12铝球,撞击速度为4.5km/s,撞击角为0°。通过固定弹丸速度、变弹丸直径、寻找弹丸临界直径的办法获得了该Whipple防护屏在试验条件下的弹道极限参数。试验结果表明速度为4.5km/s时的弹丸临界直径为0.35cm,大于用Christiansen方程预测的0.27cm。     

飞片参数与玻璃撞击损伤特征关系的研究

为考察空间碎片对航天器光学材料的影响,将光学材料撞击损伤与具体撞击碎片相对应,采用激光驱动飞片技术进行空间碎片地面模拟。设计了能形成速度可控的具体撞击碎片的激光驱动飞片装置,针对空间碎片不同速度和形态,通过改变激光能量和光束直径获得具有不同速度和长径比的飞片。研究了石英玻璃撞击损伤特征与飞片速度、长径比等参数的对应关系。结果发现:随着激光能量的增加,飞片速度的增加,撞击坑的损伤面积和坑深表现为先增大后减小;随着飞片长径比的减小,主要撞击损伤特征逐渐由侵彻成坑转变为溅射污染。通过碎片群平均参数改进为具体碎片参数,提高了地面模拟的有效性,利于高通量空间碎片环境中材料服役行为评价的研究,对空间碎片地面模拟技术和撞击损伤效应有一定的参考价值。     

航天器舷窗玻璃超高速撞击损伤与M/OD撞击风险评估

用北京卫星环境工程研究所的18mm口径二级轻气炮(TLGG)和20 J激光驱动微小飞片装置(LDFF-20)对用作航天器舷窗玻璃的熔融石英玻璃的超高速撞击损伤特性进行了实验研究和分析.其中,TLGG发射的球形铝弹丸直径分别为1 mm和3 mm,速度2～6.5 km/s;LDFF-20发射的圆柱形飞片厚度7 μm,直径1 mm,速度1～8.3 km/s.撞击结果为:对12 mm厚的熔融石英玻璃,直径为3mm的弹丸甚至在2.8 km/s的低速下就将其穿透,而直径为1 mm的弹丸在6.5km/s的高速下没有穿透,这说明弹丸直径对撞击损伤特性有很强的影响;LDFF-20发射的微小飞片的撞击仅在玻璃表面产生很浅的凹坑,没有裂纹产生,但微小飞片的累积撞击损伤明显地降低了玻璃的透光性.实验初步获得了侵彻深度PC、侵彻直径D1与弹丸撞击速度Vp、弹丸质量Mp之间的经验关系.依据实验结果和目前的微流星体/空间碎片(M/OD)环境工程模型,建议对于高度为400 km、轨道倾角42°、寿命为3年的典型航天器,其舷窗玻璃的临界安全(非穿透)厚度至少为12mm.     

用于验证数值仿真的Whipple屏超高速撞击试验结果

为提供验证超高速撞击数值仿真所需的试验结果,给出了在中国空气动力研究与发展中心超高速所进行的铝质Whipple屏超高速撞击试验部分结果。试验中,球形弹丸均为LY12铝合金材料,直径为0.4~0.5cm;靶材为间距10cm、厚0.192cm的LY12板材。撞击速度为4.47~6.15km/s,撞击角为0°和45°。给出的试验结果包括弹丸和靶材参数、撞击速度、撞击角、弹孔尺寸、后墙损伤情况和碎片云激光阴影照片等。实验结果表明,撞击速度越高,Whipple屏的防护效果越好,而斜撞击比正向撞击造成的破坏更严重。     

熔融石英玻璃超高速撞击的数值模拟与分析

熔融石英玻璃是航天器舷窗部件的主要构件,文章采用了两种计算方法(即经典的有限元算法以及新兴的sph算法)对石英玻璃受到铝球弹丸超高速(速度范围为1～10km/s)撞击后的损伤及破坏情况进行了数值模拟.通过与实验结果的比较,总结出一种较适合超高速撞击问题的计算方法,并分析了弹丸的直径及撞击速度对损伤效果的影响.     

球形弹丸超高速正撞击Whipple防护结构损伤分析

为了掌握航天器防护结构受空间碎片高速撞击的防护性能及其损伤破坏模式,采用二级轻气炮结合高速X光照相系统,对球形弹丸超高速正撞击5A06铝合金whipple防护结构进行了试验研究.根据试验结果分析了铝合金whipple防护结构的防护屏和舱壁在弹丸撞击速度为2.0-5.2km/s、弹丸直径为4mm和6.35mm及防护屏厚度为0.5film、1.5mm、2mm和3mm区间的损伤模式,总结了防护屏穿孔和舱壁损伤随弹丸撞击速度、弹丸直径以及防护屏厚度变化的规律.根据高速x光照片分析了碎片云速度和形态的变化趋势,进而从碎片云角度对舱壁损伤模式进行了分析.     

铝合金平板超高速撞击声发射信号S2模态特征分析

对铝合金平板上形成的超高速撞击(HVI)声发射(AE)信号S2模态的特征进行研究,分析其与损伤模式之间的关系。以3 mm厚5A06铝合金平板为研究对象,通过数值仿真获得不同撞击工况下的超高速撞击声发射信号,提取信号中的S2模态,并分析其幅值、能量、频谱等特征。结果表明,S2模态能量随传播距离呈指数衰减;分别随撞击弹丸直径和撞击速度的增加先下降后上升,且在弹丸直径与靶板厚度相近、临界撞击速度时最低。S2模态的中心频率随弹丸直径的增加而降低;随撞击速度的增加而增加;随传播距离的增加向1500 kHz移动。S2模态小波包系数呈凹性的频域范围分别随撞击速度和弹丸直径的增大变窄。在此基础上,当靶板形成穿孔损伤时,可根据S2模态的中心频率推测弹丸的直径;在传播距离和弹丸直径已知的前提下,可根据S2模态小波包系数呈凹性的频域范围推测撞击速度。     

圆柱体弹丸超高速斜撞击薄板的碎片云特征仿真分析

为研究圆柱体弹丸超高速撞击薄板的碎片云特征,基于仿真软件AUTODYN-3D的光滑粒子流体动力学（SPH）方法,模拟圆柱体弹丸不同长径比、不同攻角条件下超高速撞击薄板的过程。设圆柱体弹丸撞击速度为5 km/s,长径比分别为0.5、1.0、2.0、4.0,攻角为15°～75°,数值模拟结果分析表明:圆柱体弹丸超高速斜撞击薄板形成的碎片云中,大部分是小质量碎片;大碎片的质量和动能占比较大,是造成后墙损伤的主要原因。同时,当弹丸长径比为0.5和1.0时,15°攻角下的碎片云侵彻能力最弱;长径比为2.0和4.0时,75°攻角下的碎片云侵彻能力最弱。研究结果可为航天器防护结构设计优化提供参考。     

超高速撞击中的弹丸形状效应数值模拟研究

文章用AUTODYN仿真软件对球形、圆锥形、圆柱形和盘形4种不同形状弹丸超高速撞击Whipple防护结构所产生的碎片云形貌特征及对后墙的毁伤程度进行了数值仿真研究。对比分析结果指出:质量与速度相等的4种不同形状弹丸撞击缓冲屏所产生的碎片云有明显差异;弹丸长径比越小,穿过缓冲屏后的破碎程度越大;在5 km/s撞击速度下,球形弹丸对后墙的毁伤程度最小,而圆柱形弹丸的毁伤程度最大。这说明弹丸的形状对超高速撞击结果有显著影响,在航天器超高速撞击风险评估和防护工程设计中应充分考虑弹丸的形状效应。球形弹丸的弹道极限曲线在防护结构的碎片防护能力评价时存在高估的问题,在实际工作中要特别注意这一点。     

球形弹丸超高速撞击铝靶的分子动力学模拟

基于开源分子动力学程序LAMMPS建立球形铝弹丸超高速撞击铝靶的计算模型,模拟弹丸以10 km/s的速度超高速撞击单层靶、双层靶和半无限厚靶;获得了超高速碰撞靶板的物理过程及靶板损伤特性,与超高速碰撞宏观现象相似;厚靶成坑坑深与宏观经验公式计算结果基本一致。模拟结果初步表明,分子动力学方法可以对弹丸超高速碰撞薄靶和半无限厚靶进行模拟,为揭示碰撞过程中的微观机理提供了一种新的研究方法。     

Experimental hypervelocity impacts: Implication for the analysis of material retrieved after exposure to space environment: Part I. Impacts on aluminium targets

During the last three decades a wide variety of surfaces have been brought back to Earth after being exposed to space environment. The impact features found on these surfaces are used to evaluate the damages caused to spacecraft and can give clues to the characteristics of the orbital debris and meteoroids that created them. In order to derive more precisely the particle parameters and to improve the analysis of projectile remnants, we have performed an extensive analysis of craters caused by the impact of high velocity particles on thick ductile targets, using a micro-particle accelerator. We show that from the geometry of the craters and from the analysis of the remnants it is possible to derive the main characteristics of the projectiles. In particular, using up-to-date instrumentation, scanning electron microscope (SEM) and Energy Dispersive X-ray (EDX) spectrometer, we found that even small residues inside craters can be identified. However, this study shows that a velocity resolution better than 1 km/s would be appropriate to obtain a fair calibration of the impact processes on a ductile target. This would allow to decipher with precision impact features on ductile surfaces exposed to space environment.     

Location and sampling of aqueous and hydrothermal deposits in martian impact craters

Do large craters on Mars represent sites that contain aqueous and hydrothermal deposits that provide clues to astrobiological processes? Are these materials available for sampling in large craters? Several lines of evidence strongly support the exploration of large impact craters to study deposits important for astrobiology. The great depth of impact craters, up to several kilometers relative to the surrounding terrain, can allow the breaching of local aquifers, providing a source of water for lakes and hydrothermal systems. Craters can also be filled with water from outflow channels and valley networks to form large lakes with accompanying sedimentation. Impact melt and uplifted basement heat sources in craters > 50 km in diameter should be sufficient to drive substantial hydrothermal activity and keep crater lakes from freezing for thousands of years, even under cold climatic conditions. Fluid flow in hydrothermal systems is focused at the edges of large planar impact melt sheets, suggesting that the edge of the melt sheets will have experienced substantial hydrothermal alteration and mineral deposition. Hydrothermal deposits, fine-grained lacustrine sediments, and playa evaporite deposits may preserve evidence for biogeochemical processes that occurred in the aquifers and craters. Therefore, large craters may represent giant Petri dishes for culturing preexisting life on Mars and promoting biogeochemical processes. Landing sites must be identified in craters where access to the buried lacustrine sediments and impact melt deposits is provided by processes such as erosion from outflow channels, faulting, aeolian erosion, or excavation by later superimposed cratering events. Very recent gully formation and small impacts within craters may allow surface sampling of organic materials exposed only recently to the harsh oxidizing surface environment.     

超高速撞击下PTFE/Al含能材料薄板的载荷特性分析

不同于传统惰性材料的空间碎片防护结构,含能材料防护结构在超高速撞击下的冲击起爆特性是其防护能力得以提高的根本原因。PTFE/Al含能材料防护结构的冲击起爆特性改变了弹丸强冲击载荷下的破碎机制,弹丸内部的冲击压力对于分析含能材料在超高速撞击下的防护机理具有重要意义。对超高速撞击试验中回收的PTFE/Al防护结构后板进行损伤特性分析,获得了对应速度条件下弹丸的破碎特性。基于一维冲击波理论,分析PTFE/Al靶板在超高速撞击条件下的冲击响应过程,结合考虑化学反应效率的热化学反应模型,获得了弹丸在碰撞与爆炸联合作用下的载荷特性,通过与试验结果对比验证,获得该材料完全反应的临界撞击速度约为1800 m/s,弹丸的临界破碎速度为2875 m/s,小于铝防护结构中对应的临界破碎速度。给出了弹丸在PTFE/Al、铝两种防护结构中产生相同冲击压力时对应的临界速度,分别为弹道段的800 m/s和破碎段的3580 m/s。     

Impacts and evolution: future prospects

The discipline of astrobiology includes the dynamics of biological evolution. One of the major ways that the cosmos influences life is through the catastrophic environmental disruptions caused when comets and asteroids collide with a planet. We now recognize that such impacts have caused mass extinctions and played a major role in determining the evolution of life on Earth. The time-averaged impact flux as a function of projectile energy can be derived from lunar cratering statistics as well as the current population of near Earth asteroids (NEAs). Effects of impacts of various energies can be modeled, using data from historic impacts [such as the Cretaceous-Tertiary (KT) impactor 65 million years ago] and the observed 1994 bombardment of Jupiter by fragments of Comet Shoemaker-Levy 9. It is of particular interest to find from such models that the terrestrial environment is highly vulnerable to perturbation from impacts, so that even such a small event as the KT impact (by a projectile 10-15 km in diameter) can lead to a mass extinction. Similar considerations allow us to model the effects of still smaller (and much more likely) impacts, down to the size of the asteroid that exploded over Tunguska in 1908 (energy approximately 10 megatons). Combining the impact flux with estimates of environmental and ecological effects reveals that the greatest contemporary hazard is associated with impactors near 1 million megatons in energy (approximately 2 km in diameter for an asteroid). The current impact hazard is significant relative to other natural hazards, and arguments can be developed to illuminate a variety of public policy issues. The first priority in any plan for defense against impactors is to survey the population of Earth-crossing NEAs and project their orbits forward in time. This is the purpose of the Spaceguard Survey, which has already found more than half of the NEAs >1 km in diameter. If there is an NEA on a collision course with Earth, it can be discovered and the impact predicted with decades or more of warning. It is then possible to consider how to deflect or disrupt the NEA. Unlike other natural hazards, the impact risk can be largely eliminated, given sufficient advanced knowledge to take action against the threatening projectile.     

High velocity impact characterization of Al alloys for oblique impacts

This paper describes the experimental and computational analyses of a high velocity aluminum projectile impact on an Al6061-T6 spacecraft inner wall at different oblique angles. Al2017-T4 spherical projectiles of 5.56 mm in diameter and 0.25 g in weight were chosen within the velocity range of 1000±200 m/s due to the limitation of the light gas gun. The energy absorbed was calculated by measuring the velocities before and after impact on the inner wall. The energy absorbed by the wall and the remaining energy carried by the projectile helped to estimate the severity of further damage to inner components. Afterwards, validation was done by using the commercially available software LS-DYNA with a dedicated SPH. On average, a 10% energy absorption difference between experimentation and simulation was found. By using C-SCAN, the damage area proportion of the total inner wall to impact penetration hole area was found to be on average 6%, 26% and 53% greater than the projectile cross sectional area for the oblique angle impacts of 30°, 45°, and 60°, respectively. These findings helped to understand the relationship between the oblique impact event and the damage area on a spacecraft inner wall along with space debris cloud propagation and comparison with experimental results using LS-DYNA.     

Al/Mg阻抗梯度材料超高速撞击机理数值仿真研究

文章采用数值仿真方法研究了Al/Mg阻抗梯度材料在超高速撞击下的响应过程,分析了冲击波在阻抗梯度材料中的传播规律,计算了撞击过程中的能量耗散情况,并与弹丸撞击铝合金靶的结果进行了比较。研究结果表明,相对于铝合金材料,Al/Mg阻抗梯度材料：1）延长了冲击波的传播时间,使峰值压力脉冲的比冲量提升了30%～50%;2）提高了塑性功和内能转化量,使不可逆功增加了10%。由此证明阻抗梯度材料的防护性能优于铝合金。