飞行模拟器飞行指引系统控制器的设计

在现代飞机中，飞行指引系统对飞机的起飞，着陆，预选飞行高度和航向、保持飞行状态和航线飞行等方面起着十分重要的作用，它能向驾驶员提供飞机的姿态指令信号，从而确保了飞机的安全，提出了飞行效率和减轻了驾驶员飞行中的负担。本文主要讨论民机飞行模拟器中的飞行指引系统控制器的设计。     

局部可观测理论在INS/GPS机动对准中的应用

从研究INS/GPS(Inertial Navigation System/Global Positioning System)组合系统的姿态角误差可观测性出发,首次将局部可观测性理论应用于INS/GPS组合系统,定量地计算出各种不同机动方式的局部可观测矩阵的条件数,找到了提高姿态角误差可观测性的最佳机动方式.研究结果表明,通过载体做正弦水平机动飞行可以提高姿态角误差局部可观测性,使空中对准时间明显减少,姿态角误差大大降低.当对准时间为120 s时,东北天向姿态角误差的均值分别为12.34″,12.19″和-28.31″,它们的均方根值分别为0.97″,1.05″和0.62″.      

PINS静基座对准中的理论与算法的研究

分析了平台式惯导系统(PINS)静基座条件下的可观测性,采用系统可观测矩阵的条件数来定量计算PINS静基座可观测性能,找出该条件下的可观测矩阵条件数最小的3个不可观测变量.采用了自适应Kalman算法和常规Kalman算法对简化模型进行了仿真比较.仿真结果表明前者比后者滤波收敛快.进而提出了一种基于Elman神经网络的快速对准方法.     

Fractal Structure of the Heliospheric Plasma Sheet at the Earth''''s Orbit

An analysis of the data from the Wind and IMP-8 spacecraft revealed that a slow solar wind, flowing in the heliospheric plasma sheet, represents a set of magnetic tubes with plasma of increased density (N > 10cm-3 at the Earth's orbit). They have a fine structure at several spatial scales (fractality), from 2°-3°(at the Earth's orbit, it is equivalent to 3.6-5.4h, or (5.4-8.0)×106km) to the minimum about 0.025°, i.e. the angular size of the nested tubes is changed nearly by two orders of magnitude. The magnetic tubes at each observed spatial scale are diamagnetic, i.e. their surface sustains a flow of diamagnetic (or drift) current that decreases the magnetic field within the tube itself and increases it outside the tube. Furthermore, the value of β= 8π[N(Te + Tp)]/B2 within the tube exceeds the value of βoutside the tube. In many cases total pressure P = N(Te + Tp) + B2/8πis almost constant within and outside the tubes at any one of the aforementioned scales.     

Ionospheric Effects of Geomagnetic Storms in Different Longitude Sectors

This paper analyzes the state of the ionosphere during two geomagnetic storms of a different intensity evolving in different sectors of local time in different seasons. There were used the data from a network of ionospheric stations located in the opposite longitudinal sectors of 80°-150° E and 250°-310° E.This analysis has permitted us to conclude that the detected differences in the variations of the disturbances are likely to be determined by the local time difference of the geomagnetic storm development, its intensity and by the different illumination conditions of the ionosphere.      

基于改进蚁群算法的低空突防航迹规划

为保证低空突防的成功率,在航迹规划时必须设计出以最小的被发现概率及可接受的航程为目标的航迹.蚁群算法ACA(Ant Colony Algorithm)作为一种新型的模拟进化算法,适合用于航迹规划中最优航迹的搜索,但是算法存在搜索时间长、收敛速度慢、易陷于局部最优解的缺点,为了克服算法自身不足,提高算法性能,引入了遗传算法中变异操作和挥发系数的自适应调节,从而形成改进蚁群算法,最后结合建立的航迹规划性能指标,利用等概率寻优、原有蚁群算法和改进蚁群算法3种方法分别进行航迹规划,并通过比较和分析结果的时间花费和航路代价,验证了改进蚁群算法的有效性.      

Non-Thermal Processes in Cosmological Simulations

Non-thermal components are key ingredients for understanding clusters of galaxies. In the hierarchical model of structure formation, shocks and large-scale turbulence are unavoidable in the cluster formation processes. Understanding the amplification and evolution of the magnetic field in galaxy clusters is necessary for modelling both the heat transport and the dissipative processes in the hot intra-cluster plasma. The acceleration, transport and interactions of non-thermal energetic particles are essential for modelling the observed emissions. Therefore, the inclusion of the non-thermal components will be mandatory for simulating accurately the global dynamical processes in clusters. In this review, we summarise the results obtained with the simulations of the formation of galaxy clusters which address the issues of shocks, magnetic field, cosmic ray particles and turbulence.     

大气层内拦截弹脉冲姿控发动机快响应控制

气动控制在低动压时其效率会有相当下降,为了使导弹在低动压时仍然具有一定的快速响应性,在导弹上安装脉冲姿控发动机参与姿态控制是一条可行的途径.对此方法的应用作了初步研究.分析了脉冲发动机作用对导弹动力学的影响,在一系列的简化后设计了俯仰平面内的控制策略,其设计思想是用气动舵平衡气动力矩使总的气动力矩为零,使导弹姿态主要由脉冲姿控发动机来控制,并用俯仰角的变化代替攻角的变化设计脉冲姿控发动机控制策略.给出了对阶跃加速度指令的响应仿真结果,表明在具有足够动压时气动控制仍可同脉冲姿控发动机控制媲美,而在低动压时脉冲姿控发动机相对气动控制具有较大优势.      

1994年2月21日行星际激波引起的磁暴

利用Imp-8,Geotail和Goes-6等卫星资料,研究了1994年2月21日0900UT到达地球磁层的行星际激波引起的磁暴期间,从太阳风向磁层传输能量的有关问题.结果指出:（1）南向行星际磁场（IMF）的长持续时间不是太阳风向磁层输能的必要条件.南北振荡的,较强IMF也能产生显著的能量传输;（2）行星际扰动磁场通过弓激波和磁层顶后扰动磁能增加,增幅将近5倍;（3）在磁层内扰动磁场的Bz分量在1×10-4Hz附近显著被吸收.这一低频扰动磁场可能是磁暴期间导致氧离子和质子等环电流粒子向内扩散并被加速的原因之一.     

神经网络在下颌运动轨迹图测量中的应用

介绍了采用小型磁石测量下颌运动轨迹图Electrognathography(EGN)的方法。给出利用磁偶极子模型代替小磁石模型的理论及实际依据。利用神经网络解决由磁石产生的磁感应强度推定其空间参数的反演问题 ,并且采用了分割网络及修正网络的方法来提高磁石运动测量的推定准确度。