The Cassini Cosmic Dust Analyzer

The Cassini-Huygens Cosmic Dust Analyzer (CDA) is intended to provide direct observations of dust grains with masses between 10⁻¹⁹ and 10⁻⁹ kg in interplanetary space and in the jovian and saturnian systems, to investigate their physical, chemical and dynamical properties as functions of the distances to the Sun, to Jupiter and to Saturn and its satellites and rings, to study their interaction with the saturnian rings, satellites and magnetosphere. Chemical composition of interplanetary meteoroids will be compared with asteroidal and cometary dust, as well as with Saturn dust, ejecta from rings and satellites. Ring and satellites phenomena which might be effects of meteoroid impacts will be compared with the interplanetary dust environment. Electrical charges of particulate matter in the magnetosphere and its consequences will be studied, e.g. the effects of the ambient plasma and the magnetic field on the trajectories of dust particles as well as fragmentation of particles due to electrostatic disruption.The investigation will be performed with an instrument that measures the mass, composition, electric charge, speed, and flight direction of individual dust particles. It is a highly reliable and versatile instrument with a mass sensitivity 10⁶ times higher than that of the Pioneer 10 and 11 dust detectors which measured dust in the saturnian system. The Cosmic Dust Analyzer has significant inheritance from former space instrumentation developed for the VEGA, Giotto, Galileo, and Ulysses missions. It will reliably measure impacts from as low as 1 impact per month up to 10⁴ impacts per second. The instrument weighs 17 kg and consumes 12 W, the integrated time-of-flight mass spectrometer has a mass resolution of up to 50. The nominal data transmission rate is 524 bits/s and varies between 50 and 4192 bps.This revised version was published online in July 2005 with a corrected cover date.     

Cassini Imaging Science: Instrument Characteristics And Anticipated Scientific Investigations At Saturn

The Cassini Imaging Science Subsystem (ISS) is the highest-resolution two-dimensional imaging device on the Cassini Orbiter and has been designed for investigations of the bodies and phenomena found within the Saturnian planetary system. It consists of two framing cameras: a narrow angle, reflecting telescope with a 2-m focal length and a square field of view (FOV) 0.35^∘ across, and a wide-angle refractor with a 0.2-m focal length and a FOV 3.5^∘ across. At the heart of each camera is a charged coupled device (CCD) detector consisting of a 1024 square array of pixels, each 12 μ on a side. The data system allows many options for data collection, including choices for on-chip summing, rapid imaging and data compression. Each camera is outfitted with a large number of spectral filters which, taken together, span the electromagnetic spectrum from 200 to 1100 nm. These were chosen to address a multitude of Saturn-system scientific objectives: sounding the three-dimensional cloud structure and meteorology of the Saturn and Titan atmospheres, capturing lightning on both bodies, imaging the surfaces of Saturn’s many icy satellites, determining the structure of its enormous ring system, searching for previously undiscovered Saturnian moons (within and exterior to the rings), peering through the hazy Titan atmosphere to its yet-unexplored surface, and in general searching for temporal variability throughout the system on a variety of time scales. The ISS is also the optical navigation instrument for the Cassini mission. We describe here the capabilities and characteristics of the Cassini ISS, determined from both ground calibration data and in-flight data taken during cruise, and the Saturn-system investigations that will be conducted with it. At the time of writing, Cassini is approaching Saturn and the images returned to Earth thus far are both breathtaking and promising.This revised version was published online in July 2005 with a corrected cover date.     

回流燃烧室流动特性试验

为了揭示有/无燃烧状态下燃烧室热态和冷态流场的特征和流动特性,针对某型回流燃烧室单头部试验件,使用粒子图像测速仪（PIV）,测量燃烧室燃烧状态下不同截面处的热态流场,以及没有燃烧状态下不同截面处的冷态流场,探讨不同总压损失系数对回流燃烧室热态/冷态流场特征及流动特性的影响。研究表明:随着总压损失系数的增大,冷态条件下各截面流场结构基本保持不变,如射流孔穿透深度、射流角度、回流区位置及大小、流线等基本保持一致,但是各位置点速度大小逐渐增大。热态条件下各截面流场随着总压损失系数增大,流场结构也基本保持不变;相同总压损失系数时,热态流场与冷态流场存在差异,燃油喷射与气流的相对运动将会对燃烧室头部的流场结构造成影响,速度较冷态流动时略微增大。      

连续式风洞二喉道调节马赫数控制策略

为了降低连续式跨超声速风洞压力波动,提高马赫数稳定性,需要对二喉道调节马赫数控制方式进行研究,针对现有文献鲜少对该控制策略描述等问题,以0.6m连续式跨声速风洞为例,对二喉道控制马赫数的原理进行分析,基于运动控制器加伺服驱动器双PID(proportion-integral-derivative)控制模式实现二喉道位置精确控制,提出了二喉道和压缩机转速的组合控制流程,并采用分段变参数模糊PID加串级控制的算法实现马赫数精确控制,最后进行了试验验证。结果表明马赫数控制精度优于0.001,且每个马赫数极曲线(9个攻角阶梯)的时间可控制在4min以内,证明所提出的控制策略是有效的,可为连续式跨超声速风洞的设计调试提供参考。      

偏心撞击对撞击式喷嘴雾化特性的影响

为研究偏心撞击对撞击式喷嘴雾化特性的影响,建立了求解自燃推进剂冷态射流撞击雾化过程的数值模拟方案,计算了不同偏心度条件下的射流撞击雾化过程。采用树形自适应加密算法直接求解不可压Navier-Stokes方程组,由分段线性的流体体积(VOF)方法对流体界面进行捕捉。结果表明偏心撞击会导致雾场发生偏转,当无量纲偏心度E为1/8时,雾场偏转角度约为9.2°,应控制加工偏差小于该值。随着偏心度的增大,液膜的偏转角度增大,理论推导得到的液膜偏转角度要小于数值计算得到的液膜偏转角度。正心撞击时燃料与氧化剂流强峰值接近,雾场的流强分布呈单峰分布。当发生偏心撞击时,由于燃料与氧化剂部分射流未参与撞击导致流强峰值出现交错,雾场的流强分布呈双峰分布,混合比的空间分布发生较大改变。正心撞击时撞击点下游液滴的速度分布近似呈轴对称分布,而偏心撞击之后的速度分布则呈中心对称分布。偏心撞击导致的射流动量损失使得雾化性能变差,当无量纲偏心度E为1/8时,一甲基肼(MMH)的Sauter平均直径增大约4.8%,四氧化二氮(NTO)的Sauter平均直径增大约5.8%。      

基于点云数据的发动机管路最小间距计算方案

为检测整机发动机管路是否满足最小间距的设计要求,提出了一种基于点云数据的发动机管路最小间距计算方案,方案包含5个步骤:①从点云数据中划分出不同管路的数据;②基于管路点云数据的空间分布构造等间隔栅格,计算栅格中心点作为管路的趋势线数据;③在管路各趋势线数据点位置上构造垂直平面,将管路点云数据投影到最近的垂直平面上,获得各个垂直平面上呈圆弧状分布的投影点数据;④对各垂直平面上的投影点数据进行最小二乘圆拟合,得到拟合圆圆心及其半径值,将拟合圆圆心作为管路中心线数据;⑤采用遍历法计算两条管路中心线数据的最小间距,中心线最小间距分别减去两条管路的半径值则得到两条管路的表面最小间距。通过12条管路验证了方案的准确度。实验结果表明:管路最小间距偏差在-0.35~0.46mm之间,管路半径偏差在-0.08~0.22mm之间。该方案的实施有助于管路间距数字化检测的实现,且方案的计算结果具有较好的鲁棒性。      

基于卷积门控循环网络的滚动轴承故障诊断

针对许多基于深度学习的滚动轴承故障诊断方法在小样本数据集下诊断性能下降的问题,提出一种基于卷积门控循环神经网络的轴承故障诊断模型。该模型使用两层的卷积网络来从输入信号中提取特征,同时使用tanh函数作为激活函数,且池化层使用大池化核来进行重叠下采样。将所提取得到的高层特征连接到双向门控循环网络。合并循环网络正向和逆向的最后一个状态,并连接一层全连接层进行输出。选用凯斯西储大学的轴承故障数据集来验证模型在小样本数据集下的诊断性能,实验结果表明,相比于其他类型的模型,该模型在仅有20个训练样本的情况下依然保持97%的识别准确率。      

不同转速下自循环机匣处理对转子性能的影响

以NASA Rotor 37为研究对象,采用数值模拟的方法研究了自循环机匣处理的引气位置在不同转速下对转子性能的影响。研究结果表明:自循环机匣处理的引气位置和转子转速对转子性能的影响具有交互性,其本质原因在于转子在不同转速下处于近失速状态时,转子叶顶区域的流动状态不同,从而造成引气位置和叶顶堵塞区域的相对位置会随着转子转速的变化而变化,进而对转子的性能影响呈现出交互性。通过对三种转速下自循环机匣处理的引气位置对转子稳定性的影响分析知,引气位置位于转子叶顶堵塞区尾缘处时对转子叶顶区的流动堵塞抑制能力最强,极大地改善了转子叶顶区域的流通状况,对转子的失速裕度改进量最为有利,在100%、90%和70%设计转速下,失速裕度改进量的最大值分别为7.46%、8.52%、6.14%。此外,通过对转子叶顶的流场细节分析得知,不同转速下自循环机匣处理的引气位置位于转子近失速工况的叶顶堵塞区尾缘处时,在叶顶造成的高比熵区最少,对转子效率的降低幅度最小,于效率最为有利。      

陀螺经纬仪在大型航天产品精测中的应用

陀螺经纬仪通常是做某一方向与当地大地北向的方位角关系测量用。文章针对“天宫一号”目标飞行器精测中遇到的问题,即高空不同平台间两台设备需要姿态关系测量的需求,通过对陀螺经纬仪测量原理的研究,借助大地坐标系作为中间传递坐标系,解决了经纬仪测量因互瞄被遮挡无法建立基准镜坐标系间关系的问题。测量误差分析结果验证了这种新方法的可行性,该方法可用于大型航天产品设备安装精度的测量。     

首次交会对接任务发射场加注安全保障改进

载人航天器加注是航天器研制过程中安全风险最高、危险作业工序最多的环节,必须采取严密的安全防护措施,确保万无一失.通过实践探索积累经验,全面周密的设计论证,对原有加注硬件条件进行改造,工作流程进行优化,从而大幅提高本质安全度,并在首次交会对接任务中加以应用和验证,取得了良好的效果,圆满完成了“天宫一号”、“神舟八号”发射...