基于改进蚁群算法的无人机三维航路规划

针对蚁群算法存在收敛速度慢,容易陷入局部最优而导致三维航路规划过程中出现规划时间过长、航路没有达到最优等问题,通过对蚁群算法进行改进,提出了一种天牛须融合改进蚁群的无人机航路规划优化算法,算法通过对蚁群算法的启发函数优化并进行蚁群择优排序,然后融合天牛须算法进行航路规划;将优化算法应用于无人机的三维航路规划中,使规划算法的运行速度更快,无人机的最优航路更短。同时用改进算法与天牛须、蚁群算法的收敛时间、最优路径长度进行对比。仿真实验结果表明,改进算法与另外两种算法相比,在算法收敛度、运行速度方面有明显的提升。     

基于改进MeanShift算法的视线跟踪技术

介绍了SURF算法和MeanShift算法的基本原理。将MeanShift跟踪算法应用于视觉鼠标技术,提出了基于OpenCV技术的视线系统设计方法;提出了基于SURF算法的自动嘴部区域初始化MeanShift改进算法。实验结果表明,算法匹配识别效果较好,基于MeanShift跟踪算法的嘴唇跟踪系统实时性好、具有较好鲁棒性。     

飞行轨迹预测的两种变结构IMM算法

针对交互式多模型(IMM)算法的缺陷,把变结构思想运用到此算法中,给出变结构交互式多模型(VSIMM)算法。基于图论知识,提出两种变结构算法:转换图交互式多模型(SGIMM)算法和自适应图交互式模型(AGIMM)算法。通过仿真试验,验证了这2种变结构算法的优越性,同时分析了2种算法的不同点。     

低空无人机路径规划算法综述

随着无人机技术的发展,无人机在低空的应用场景越来越多,复杂的低空环境对无人机路径规划算法提出了新的要求。本文总结了近年来常用的无人机路径规划算法,包括图搜索算法,线性规划算法,智能优化算法（遗传算法、粒子群算法、蚁群算法）,强化学习算法;对这些算法的原理、适用场景及其优缺点进行了归纳分析;并基于无人机发展现状对无人机路径规划算法进行了展望。     

自适应DR算法研究

首先介绍了 DR算法的基本思想 ,并分析了现有的 DR算法的不足之处。然后提出了一种自适应 DR算法。最后 ,将提出的这种自适应 DR算法与普通 DR算法进行了比较研究。结果表明 ,自适应 DR算法是十分有效的     

利用实乘子实现快速FFT算法研究

引入实乘子的算法代替传统复乘子来实现快速傅立叶变换。给出了该实乘子算法的详细推导过程,结合同址计算的原理给出了算法流程。并列出了此算法与传统的DFT算法的运算量的比较,看出此算法的高效性。指出了该算法在调频引信变频处理中的重要应用。     

UKF-WNN及其在准定常失速气动力建模中的应用

提出一种利用无轨迹卡尔曼滤波估计小波网络参数的算法,该算法可克服算法存在的收敛速度慢、计算量大、局部极小等缺点。以飞机的准定常失速现象的气动力建模为应用背景,分别运用BP算法,扩展卡尔曼滤波算法和无轨迹卡尔曼滤波算法训练小波网络。仿真结果表明,无轨迹卡尔曼滤波算法较之BP算法和扩展卡尔曼滤波算法具有更快的训练速度和更高的预测精度,可以胜任复杂的非线性气动现象的建模任务。     

超参数自适应的MOEA/D-DE算法在翼型气动隐身优化中的应用

MOEA/D-DE 算法易于实现，被广泛应用于处理多目标优化问题，但其超参数CR 和F 对算法性能影响较大。基于MOEA/D-DE 算法框架、利用Sobol 全局灵敏性分析方法对差分进化算子中的交叉控制参数CR进行改进，使用莱维飞行策略控制比例因子F，使算法中的超参数拥有自适应能力，得到超参数自适应的MOEA/D-DE 算法——MOEA/D-DEAH 算法；对MOEA/D-DEAH 算法、不同超参数设置的MOEA/D-DE算法和NSGAII 算法进行函数测试和翼型气动隐身优化算例对比。结果表明：MOEA/D-DEAH 算法性能良好，具有较强的鲁棒性，气动隐身优化效果也比其他算法更好。     

飞机起落架噪声源定位的压缩感知算法

目前针对飞机起落架噪声源定位的研究方法主要是将麦克风阵列与波束成形算法相结合。常规波束成形（CBF）算法在计算时存在主瓣宽度过宽、结果易受旁瓣影响的问题。高级波束成形算法在计算时效率较差,有时会有违背物理现象的假声源出现。提出了一种将正交匹配追踪（OMP）算法与奇异值分解（SVD）相结合的起落架噪声源定位的OMP-SVD压缩感知算法。在消声实验室内进行飞机起落架噪声源定位试验,将OMP-SVD算法、CBF算法和OMP算法在不同频率下获得的结果进行对比。试验结果表明：①与OMP算法相比,OMP-SVD算法在不同频率下均能准确定位出起落架主声源;②与CBF算法相比,OMP-SVD算法显著提高了分辨率。     

最小生成树算法及其应用

Kruskal算法和Prim算法是求最小生成树的常用算法,设计了这两种算法的C语言程序,并通过实例研究了这两种算法的实际应用价值。     

某型飞机端盖的失效分析

采用扫描电子显微镜(SEM)、能谱分析(EDS)和显微硬度(MHV)测试等手段对某型飞机的Al-Si-Cu铸造合金端盖进行了失效分析.结果表明:在交变载荷的长期作用下,端盖凸缘处材料出现了裂纹.裂纹的存在引起了应力集中,最终导致了零件的疲劳断裂.     

Review of Ionospheric Effects of Solar Wind Magnetosphere Coupling in the Context of the Expanding Contracting Polar Cap Boundary Model

This paper reviews the coupling between the solar wind, magnetosphere and ionosphere. The coupling between the solar wind and Earth’s magnetosphere is controlled by the orientation of the Interplanetary Magnetic Field (IMF). When the IMF has a southward component, the coupling is strongest and the ionospheric convection pattern that is generated is a simple twin cell pattern with anti-sunward flow across the polar cap and return, sunward flow at lower latitudes. When the IMF is northward, the ionospheric convection pattern is more complex, involving flow driven by reconnection between the IMF and the tail lobe field, which is sunward in the polar cap near noon. Typically four cells are found when the IMF is northward, and the convection pattern is also more contracted under these conditions. The presence of a strong Y (dawn-dusk) component to the IMF leads to asymmetries in the flow pattern. Reconnection, however, is typically transient in nature both at the dayside magnetopause and in the geomagnetic tail. The transient events at the dayside are referred to as flux transfer events (FTEs), while the substorm process illustrates the transient nature of reconnection in the tail. The transient nature of reconnection lead to the proposal of an alternative model for flow stimulation which is termed the expanding/contracting polar cap boundary model. In this model, the addition to, or removal from, the polar cap of magnetic flux stimulates flow as the polar cap boundary seeks to return to an equilibrium position. The resulting average patterns of flow are therefore a summation of the addition of open flux to the polar cap at the dayside and the removal of flux from the polar cap in the nightside. This paper reviews progress over the last decade in our understanding of ionospheric convection that is driven by transient reconnection such as FTEs as well as by reconnection in the tail during substorms in the context of a simple model of the variation of open magnetic flux. In this model, the polar cap expands when the reconnection rate is higher at the dayside magnetopause than in the tail and contracts when the opposite is the case. By measuring the size of the polar cap, the dynamics of the open flux in the tail can be followed on a large scale.     

Solar Wind Control of the Magnetospheric and Auroral Dynamics

A dependence of the polar cap magnetic flux on the interplanetary magnetic field and on the solar wind dynamic pressure is studied. The model calculations of the polar cap and auroral oval magnetic fluxes at the ionospheric level are presented. The obtained functions are based on the paraboloid magnetospheric model calculations. The scaling law for the polar cap diameter changing for different subsolar distances is demonstrated. Quiet conditions are used to compare theoretical results with the UV images of the Earth’s polar region obtained onboard the Polar and IMAGE spacecrafts. The model calculations enable finding not only the average polar cap magnetic flux but also the extreme values of the polar cap and auroral oval magnetic fluxes. These values can be attained in the course of the severe magnetic storm. Spectacular aurora often can be seen at midlatitude during severe magnetic storm. In particularly, the Bastille Day storm of July 15–16, 2000, was a severe magnetic storm when auroral displays were reported at midlatitudes. Enhancement of global magnetospheric current systems (ring current and tail current) and corresponding reconstruction of the magnetospheric structure is a reason for the equatorward displacement of the auroral zone. But at the start of the studied event the contracted polar cap and auroral oval were observed. In this case, the sudden solar wind pressure pulse was associated with a simultaneous northward IMF turning. Such IMF and solar wind pressure behavior is a cause of the observed aurora dynamics.     

高精度加速度计力矩器磁路的设计与仿真分析

力矩器磁路性能决定了加速度计标度因数的性能,为此利用有限元方法对力矩器磁路的磁通密度进行分析,在此基础上提出了两种结构优化设计方案,并对其进行仿真计算。仿真结果表明,改变导磁帽的形状可以提高气隙磁场的磁通密度的稳定性和均匀性,但导磁帽易出现饱和现象;通过降低磁钢的高度,同时增加导磁帽的高度,既能大幅度的提高磁场的稳定性和均匀性,导磁帽也不会出现饱和现象,但气隙磁场的磁通密度均值会降低37.25%,非线性误差为1.83%,优化后气隙磁场存在着磁通密度稳定（径向均值为0.42868T）和均匀的区域。     

超声速光学头罩流场的PIV研究

在马赫数Ma-3．8超声速风洞中,采用PIV（Particle Image Velocimetry,粒子图像测速）技术测量了超声速光学头罩流场的速度分布。PIV技术应用于超声速流场时,对系统的硬件配备、示踪粒子的跟随性以及PIV算法的精度有很高的要求。本文PIV系统选用高精度的同步控制器和高能量激光器;以纳米级粒径的粒子作为示踪粒子,通过斜激波响应实验分析了其在超声速流场中的跟随性;并采用多种高精度速度场算法对粒子图像进行处理。实验结果表明,示踪粒子在超声速流场中有很好的跟随性,采用的高精度速度场算法能够很好地反映超声速光学头罩流场的速度分布。     

Electric fields in the ionosphere and magnetosphere

In this paper we review low altitude observations of the high latitude convection electric field as obtained with a variety of instruments including polar orbiting spacecraft, barium, incoherent and coherent scatter radars, and ground-based magnetometers. There still appears to be some contradiction in the observations particularly with regard to plasma flow into and out of the polar cap. Also, there does not appear to be any simple relationship between the sign of B _y and the local time location of the throat region. Rather, under active conditions, it appears that the plasma entry and exit regions rotate towards earlier times and there is a significant component of dawn-dusk flow across the polar cap. Superimposed on this may be some B _y-dependence of the plasma entry region.     

带键槽细长轴的热处理

主要叙述带键槽细长轴热处理工艺技术与方法,特别介绍了“盖边销保护淬火”、“涂覆保护涂料”、“倾斜淬火冷却”、“渗碳去碳”等热处理成功实例.     

Experimental Aspects of Mid-Frequency Pulsations (f≈10–100 mHz) in the Southern Polar Cap

We review the results obtained in the frequency range of Pc3 (22-100 mHz) and Pc4 (7-22 mHz) pulsations at Italian Antarctic stations in the southern polar cap (“Mario Zucchelli”, at Terra Nova Bay, TNB, 80^˚.S; “Concordia”, the Italian/French base at Dome C, DMC, 89^˚.S). The absence of a midnight enhancement in the pulsation power suggests a negligible substorm influence at extreme latitudes, while the sharp noon enhancement, which appears only at TNB, is determined by the closer proximity of the station to cusp related phenomena. The relationship between the frequency of the band-limited signals and the interplanetary magnetic field strength, the cone angle influence, and the higher correlation of the Pc3 power with the solar wind speed in the morning hours suggest a global scenario in which upstream waves would be mainly responsible for the mid-frequency activity in the polar cap. However, the polarization pattern is odd with respect to the predictions for tailward propagating modes.     

超声速弹头凹型光学头罩流动显示研究

在自行设计的Ma=3．8超声速风洞中,采用基于纳米技术的平面激光散射（NPLS）方法对超声速弹头凹型光学头罩流场进行了流动显示实验。高时空分辨率的NPLS图像再现了激波、膨胀波、边界层及尾迹等流场结构。观察到了边界层的产生、发展及转捩过程。通过对时间相关图像的分析,可以精确测定边界层内大尺度结构的几何特征和时间演化特征。