悬索桥的风致振动分析

系统分析悬索桥的颤振稳定性，抖振响应和涡激共振，以Ｓｃａｎｌａｎ Ｒ Ｈ提出的分离流三维颤抖振理论和半经验非线性涡激力假设为基础，分别用频域和时域方法，建立气动弹性模型。频域中用Ｖ－ｇ法和统计方法求解颤抖振。时域中用根轨迹法确定颤振，用求解Ｌｙａｐｕｎｏｖ矩阵方程的方法确定抖振响应，通过对实际悬索桥的分析，两种方法得到了比较一致的结果。     

防止Ⅱ型驾驶员诱发振荡技术的研究

许多严重的飞行事故都与由速率限制引起的Ⅱ型PIO有关。针对如何预防PIO，首先介绍了自适应杆增益和软件限制环节的设计原理。然后以某带速率限制的电传飞机为例，运用同一理论，分析采用自适应杆增益和软件限制环节来改善速率限制的不利影响。仿真结果表明，自适应杆增益环节和软件限制环节都能抑制住PIO的发生，但两者组合加入抑制效果更好，飞行品质也能达到满意的程度。     

全权限数字电子控制器雷电试验方法研究

在分析机载设备雷电感应敏感度试验相关标准的基础上,对全权限数字电子控制器雷电间接效应试验方法进行研究。对雷电间接效应耦合方式进行了分类,并以某型全权限数字电子控制器为例,介绍了数字电子控制器雷电感应瞬态敏感度试验波形组、试验电平选择方法及试验过程。并对空客和波音公司机载设备雷电感应瞬态敏感度试验方法做了初步介绍。研究成果可供制定机载设备雷电防护要求及试验方案时参考。     

接触特性对非连续性转子热致振动的影响

针对燃气轮机转子的非连续性结构间存在的接触特性,根据微凸体理论引入接触刚度和接触热阻的等效模型,建立了某型燃气轮机非连续性转子的动力学模型,分析了接触参数对转子稳、瞬态动力学特性的影响,研究了螺栓松动引起的转子热变形及其对转子快速启动过程中振动特性的影响.结果表明:预紧力、接触面的表面粗糙度和螺栓个数对转子临界转速有一定的影响,螺栓松动导致转子在启动过程中瞬态热变形最大达到7μm,过1阶临界转速时引起的转子最大响应幅值增大约30μm.在非连续性转子系统的热致振动特性分析当中,不应忽视接触参数、接触刚度和接触热阻的影响.      

星载可展开天线热振动数值分析

根据非耦合动力学理论及有限元方法,研究分析了星载可展开天线的热振动。利用半正弦波温度冲击模拟热动力荷载,对天线典型节点的热振动位移和应力以及形面精度进行了数值分析。研究表明,急剧变化的温度荷载将导致该天线结构发生热振动,热振动响应明显大于静力学响应。     

磁静日期间中国大陆地区外源弱磁场研究

利用第四代地磁场综合模型CM4, 研究了中国大陆地区1960-2000年磁静日期间地磁外源弱磁场的变化情况, 计算并分析了外源场中的电离层感应场、环形场以及磁层感应场的分布和变化. 结果显示, 北向分量X的磁层感应场强度总体呈先增加后减少的趋势, 共减少了约7.3nT; 东向分量Y的磁层感应场强度呈先减少后增加的趋势, 共增加了约0.8nT; 垂直分量Z的磁层感应场强度呈先增加后减少的趋势, 共增加了约5.5nT. 三个分量的电离层感应场以及环形场变化幅度很小, 其分布在1960-1970和1970-1980年, 1980-1990 和1990-2000年呈现正负互相变换的现象, 认为该现象可能与太阳11年活动周期有关. 最后对弱磁场随时间变化的结果进行了分析说明.      

Are small-scale field-aligned currents and magnetosheath-like particle precipitation signatures of the same low-altitude cusp?

We examined some 75 observations from the low-altitude Earth orbiting DMSP, Ørsted and CHAMP satellites which were taken in the region of the nominal cusp. Our objective was to determine whether the actually observed cusp locations as inferred from magnetosheath-like particle precipitation (“particle cusp”) and intense small-scale magnetic field variations (“current cusp”), respectively, were identical and were consistent with the statistically expected latitude of the cusp derived from a huge number of charged particle spectrograms (“statistical cusp”).     

A Comparative Study of the Influence of the Active Young Sun on the Early Atmospheres of Earth, Venus, and Mars

Because the solar radiation and particle environment plays a major role in all atmospheric processes such as ionization, dissociation, heating of the upper atmospheres, and thermal and non-thermal atmospheric loss processes, the long-time evolution of planetary atmospheres and their water inventories can only be understood within the context of the evolving Sun. We compare the effect of solar induced X-ray and EUV (XUV) heating on the upper atmospheres of Earth, Venus and Mars since the time when the Sun arrived at the Zero-Age-Main-Sequence (ZAMS) about 4.6 Gyr ago. We apply a diffusive-gravitational equilibrium and thermal balance model for studying heating of the early thermospheres by photodissociation and ionization processes, due to exothermic chemical reactions and cooling by IR-radiating molecules like CO₂, NO, OH, etc. Our model simulations result in extended thermospheres for early Earth, Venus and Mars. The exospheric temperatures obtained for all the three planets during this time period lead to diffusion-limited hydrodynamic escape of atomic hydrogen and high Jeans’ escape rates for heavier species like H₂, He, C, N, O, etc. The duration of this blow-off phase for atomic hydrogen depends essentially on the mixing ratios of CO₂, N₂ and H₂O in the atmospheres and could last from ∼100 to several hundred million years. Furthermore, we study the efficiency of various non-thermal atmospheric loss processes on Venus and Mars and investigate the possible protecting effect of the early martian magnetosphere against solar wind induced ion pick up erosion. We find that the early martian magnetic field could decrease the ion-related non-thermal escape rates by a great amount. It is possible that non-magnetized early Mars could have lost its whole atmosphere due to the combined effect of its extended upper atmosphere and a dense solar wind plasma flow of the young Sun during about 200 Myr after the Sun arrived at the ZAMS. Depending on the solar wind parameters, our model simulations for early Venus show that ion pick up by strong solar wind from a non-magnetized planet could erode up to an equivalent amount of ∼250 bar of O⁺ ions during the first several hundred million years. This accumulated loss corresponds to an equivalent mass of ∼1 terrestrial ocean (TO (1 TO ∼1.39×10²⁴ g or expressed as partial pressure, about 265 bar, which corresponds to ∼2900 m average depth)). Finally, we discuss and compare our findings with the results of preceding studies.     

融合式翼梢小翼减阻效应研究

有效减小诱导阻力对于飞机降低油耗、提高航程具有重要意义。针对某飞机翼身组合体构型,采用CFD数值模拟方法分析融合式翼梢小翼对飞机气动力特性的影响,尤其是其减阻效应;并给出翼梢小翼附近的空间流场。结果表明:带翼梢小翼后翼尖涡强度减弱,飞机阻力系数明显下降;固定升力系数0.5时,弯矩增加3.2%,阻力系数减小4.2%。     

基于黏性涡模型的旋翼流场数值方法

 建立了一种适用于旋翼非定常流场特性分析的黏性涡数值方法。在该方法中:流场中的大尺度涡被离散为若干微小的涡元,通过求解涡量-速度形式的Navier-Stokes方程模拟涡元的输运等过程;黏性扩散效应采用高精度的粒子强度交换法进行计算,而桨叶附着涡以及新生涡环量采用了Weissinger-L升力面理论进行求解;为显著提高计算效率,在诱导速度及其梯度的计算中还引入了快速多极子算法(FMM)。应用上述方法,对悬停和前飞状态下的多个旋翼流场算例进行了计算,通过对比旋翼尾迹涡量特征和诱导速度分布等,验证了该方法的有效性。此外,还将本方法与旋翼计算流体力学(CFD)方法及传统的自由尾迹方法进行了比较,结果表明黏性涡方法在兼顾效率的同时,还能够更好地捕捉旋翼尾迹运动。