推力矢量飞机的起飞性能研究

简述推力矢量技术的作用,建立了带三轴推力矢量飞机的起飞滑跑段运动方程,通过数值仿真探讨了推力矢量的偏转大小对起飞性能的影响,对不同推力矢量偏转下飞机起飞性能的仿真计算结果进行了分析。仿真结果表明,采用直接力控制可以明显提高飞机的起飞性能。     

涡扇发动机排气系统红外特征

采用反向蒙特卡罗法(Reverse Monte-carlo,简称RMC)结合窄带模型计算了模型涡扇发动机(不带加力)排气系统的红外辐射强度。考虑了金属壁面的发射和反射以及燃气中CO2,CO和H2O等组分的吸收、发射和透射,组分的吸收系数由NASA SP3080数据库获得,并对判断射线归宿的过程进行了改进,开发了计算程序。实验测量了模型涡扇发动机排气系统的中波红外光谱辐射强度及其空间辐射强度分布。结果表明:计算得到的3～5μm波段内的光谱辐射强度以及空间辐射强度分布与实验值吻合较好,最大误差为10%左右,本文的计算方法能比较准确地反映涡扇发动机排气系统在非加力状态下的中波红外辐射特征。     

飞行监控系统中基于GPU的地形渲染

利用实时遥测飞行信息生成三维虚拟地形场景,旨在飞机试飞时,增强地面指挥人员对飞机实时位置地面场景的感知能力,帮助飞行员在试飞时处理复杂多变的飞行状况。为了逼真且流畅地生成三维地形场景,首先使用固定网格映射(PGM)的方法生成地形采样网格,接着利用几何着色器为三角形面片分配连续的与视点相关的细节等级(LOD),对缓存在纹理数组中的各等级高程数据和卫星照片进行混合采样。由于细节等级是连续的,因此各级纹理和高程之间能够平滑的过渡,增加了场景的真实性。最后,考虑到显存的容量限制,引入了一种内存与显存之间的纹理调度方法。整个算法都是面向图形处理单元(GPU)实现的,能够较好地兼顾实时性和真实性,实现多分辨率大规模地形场景的实时虚拟显示。根据本文算法实现的实时监控系统在支线飞机的飞行试验中取得了较好的效果。     

Erosion of a Polyimide Material Exposed to Simulated Atomic Oxygen Environment

Oxygen plasma source generated by thermal cathode filament discharge has been used to study the erosion process of polyimide (PI) materials in atomic oxygen (AO) environment, and their mass loss, surface morphology and surface chemical compositions have been examined by scanning electron microscope (SEM) and X-ray photoelectron spectroscopy (XPS) after exposure to incremental AO flux. The data indicate that the physical adsorption of AO at the samples' surface results in the increase of oxygen concentration when polyimide is exposed to AO flux. Then selective chemical reactions of groups of polyimide materials with AO yield volatile organic compounds, sample mass loss is on linear increase and carpet-like surface morphology forms. In the initial exposure to AO, the reaction occurs mainly between AO and carbon in specific location of aromatic ring, then the reaction rate of C=O groups gradually increases. After AO exposure, the oxygen concentration increases while nitrogen and carbon concentration decreases. Reaction rate of groups containing nitrogen is slower compared with carbon and oxygen.     

基于二叉树支持向量机的装备故障诊断研究

本文提出了一种基于二叉树支持向量机的某型装备故障诊断方法,应用该方法构造了多故障分类器,并通过某型装备故障实例验证了该方法故障诊断结果的正确性,证明了该故障诊断方法具有良好的鲁棒性和推广性。     

应用加工硬化率研究TA15钛合金β区变形的动态再结晶临界条件

基于位错理论探讨了材料大应变条件下的加工硬化率曲线及动态再结晶的拐点判据,利用在变形温度1050～1100℃、应变速率0.001～1s-1条件下等温恒应变速率压缩试验获得的应力-应变数据,采用加工硬化率处理方法,研究了TA15钛合金β区变形的动态再结晶临界条件,并应用Zener-Hollomon参数建立了临界应变模型。结果表明,TA15钛合金在本试验条件下呈现两种曲线特征类型的应力-应变曲线,其θ-σ曲线均呈现拐点及-θ/σ-σ曲线上出现最小值;临界应变与峰值应变之间具有一定的相关性,即εc/εp=0.62;临界应变与Z参数之间的函数关系为εc=1.72×10-2Z0.0605。     

基于傅里叶变换的航迹对准关联算法

研究了在组网雷达存在系统误差情况下的目标航迹关联问题,理论分析了雷达系统误差对目标航迹的影响,并将该影响表示为目标航迹的旋转和平移量。在此基础上,提出了一种基于傅里叶变换的系统误差配准前航迹对准关联算法,该算法将组网雷达的航迹数据看做为一种整体信息,采用傅里叶变换理论来估计和补偿组网雷达目标航迹数据到融合中心航迹数据的相对旋转量和平移量,将雷达网中雷达上报的目标航迹数据对准到融合中心,从而不依赖于估计雷达网系统误差,实现了误差配准前的航迹准确关联,能够为后端的系统误差配准提供可靠的关联目标航迹数据。     

某型飞机铝合金LY11螺旋桨腐蚀损伤试验

在疲劳试验机及电磁激振试验台上,对不同腐蚀情况的某型飞机螺旋桨桨叶模拟试件进行试验,分别得到了腐蚀损伤面积比随低周循环数N的变化规律,振动频率随损伤深度比、损伤长度比及损伤面积比的变化规律.试验表明,在载荷、温度相同条件下,材料性能、喷丸强化措施和使用环境是影响螺旋桨腐蚀损伤的重要因素;腐蚀损伤的面积比、腐蚀深度比对螺旋桨桨叶振动频率影响较大并获得最大深度比为0.14,模拟试件损伤深度最大允许值为0.7 mm,损伤面积比为0.015,损伤面积最大允许值为3.006 mm2.      

船用燃气轮机间冷器流路的数值计算分析

借助计算流体动力学(CFD)数值模拟技术,实现了船用燃气轮机间冷器整个流路的总压损失分析.数值模拟计算中针对间冷器模块采用了等效流通面积和等效换热效果的方法,有效解决了整个流道计算间冷器建模问题.数值模拟计算结果表明,CFD数值模拟技术可以有效的分析包括间冷器在内的整个流路的流场细节,改善间冷器的流路设计.CFD数值模拟技术与间冷换热器设计技术的结合,可以有效提高船用燃气轮机间冷器整个流路的优化设计水平.      

Magnetosphere Imaging Instrument (MIMI) on the Cassini Mission to Saturn/Titan

The magnetospheric imaging instrument (MIMI) is a neutral and charged particle detection system on the Cassini orbiter spacecraft designed to perform both global imaging and in-situ measurements to study the overall configuration and dynamics of Saturn’s magnetosphere and its interactions with the solar wind, Saturn’s atmosphere, Titan, and the icy satellites. The processes responsible for Saturn’s aurora will be investigated; a search will be performed for substorms at Saturn; and the origins of magnetospheric hot plasmas will be determined. Further, the Jovian magnetosphere and Io torus will be imaged during Jupiter flyby. The investigative approach is twofold. (1) Perform remote sensing of the magnetospheric energetic (E > 7 keV) ion plasmas by detecting and imaging charge-exchange neutrals, created when magnetospheric ions capture electrons from ambient neutral gas. Such escaping neutrals were detected by the Voyager l spacecraft outside Saturn’s magnetosphere and can be used like photons to form images of the emitting regions, as has been demonstrated at Earth. (2) Determine through in-situ measurements the 3-D particle distribution functions including ion composition and charge states (E > 3 keV/e). The combination of in-situ measurements with global images, together with analysis and interpretation techniques that include direct “forward modeling’’ and deconvolution by tomography, is expected to yield a global assessment of magnetospheric structure and dynamics, including (a) magnetospheric ring currents and hot plasma populations, (b) magnetic field distortions, (c) electric field configuration, (d) particle injection boundaries associated with magnetic storms and substorms, and (e) the connection of the magnetosphere to ionospheric altitudes. Titan and its torus will stand out in energetic neutral images throughout the Cassini orbit, and thus serve as a continuous remote probe of ion flux variations near 20R _S (e.g., magnetopause crossings and substorm plasma injections). The Titan exosphere and its cometary interaction with magnetospheric plasmas will be imaged in detail on each flyby. The three principal sensors of MIMI consists of an ion and neutral camera (INCA), a charge–energy–mass-spectrometer (CHEMS) essentially identical to our instrument flown on the ISTP/Geotail spacecraft, and the low energy magnetospheric measurements system (LEMMS), an advanced design of one of our sensors flown on the Galileo spacecraft. The INCA head is a large geometry factor (G ∼ 2.4 cm² sr) foil time-of-flight (TOF) camera that separately registers the incident direction of either energetic neutral atoms (ENA) or ion species (≥5^∘ full width half maximum) over the range 7 keV/nuc < E < 3 MeV/nuc. CHEMS uses electrostatic deflection, TOF, and energy measurement to determine ion energy, charge state, mass, and 3-D anisotropy in the range 3 ≤ E ≤ 220 keV/e with good (∼0.05 cm² sr) sensitivity. LEMMS is a two-ended telescope that measures ions in the range 0.03 ≤ E ≤ 18 MeV and electrons 0.015 ≤ E≤ 0.884 MeV in the forward direction (G ∼ 0.02 cm² sr), while high energy electrons (0.1–5 MeV) and ions (1.6–160 MeV) are measured from the back direction (G ∼ 0.4 cm² sr). The latter are relevant to inner magnetosphere studies of diffusion processes and satellite microsignatures as well as cosmic ray albedo neutron decay (CRAND). Our analyses of Voyager energetic neutral particle and Lyman-α measurements show that INCA will provide statistically significant global magnetospheric images from a distance of ∼60 R _S every 2–3 h (every ∼10 min from ∼20 R _S). Moreover, during Titan flybys, INCA will provide images of the interaction of the Titan exosphere with the Saturn magnetosphere every 1.5 min. Time resolution for charged particle measurements can be < 0.1 s, which is more than adequate for microsignature studies. Data obtained during Venus-2 flyby and Earth swingby in June and August 1999, respectively, and Jupiter flyby in December 2000 to January 2001 show that the instrument is performing well, has made important and heretofore unobtainable measurements in interplanetary space at Jupiter, and will likely obtain high-quality data throughout each orbit of the Cassini mission at Saturn. Sample data from each of the three sensors during the August 18 Earth swingby are shown, including the first ENA image of part of the ring current obtained by an instrument specifically designed for this purpose. Similarily, measurements in cis-Jovian space include the first detailed charge state determination of Iogenic ions and several ENA images of that planet’s magnetosphere.This revised version was published online in July 2005 with a corrected cover date.