飞机非线性飞行载荷计算方法研究

 以贯彻《军用飞机强度和刚度规范》为目标,提出了一整套使用风洞实验非线性气动力数据进行飞机飞行载荷计算的方法,成功地研制了带有载荷数据库的计算分析软件。该软件已成功地运用于 F××飞机的飞行载荷计算。     

两种气动布局飞机的着陆特性分析

应用 2种气动布局飞机在着陆构形下的气动力数据 ,仿真计算了飞机的进场着陆过程 ,通过对着陆性能与飞行品质的分析表明 ,飞机气动特性和飞行员的操纵策略对着陆性能起着重要的作用。     

大尖削机翼非定常跨音速绕流的数值解法(英文)

本文给出一种计算飞机机翼上定常和非定常跨音速气动力的数值解法,使用了一种特殊设计的坐标变换,是用时间精确交替方向隐式(ADI)有限差分算法来求解非定常跨音速修正三元小扰动位势方程。给出了F5战斗机机翼的数值结果并与XTRAN3S,ATRAN3S及试验结果进行了比较,表明本方法是有效的和经济的。     

涡流管结构参数对其性能的影响

用实验方法研究了热端管管长、分离室直径、冷孔板孔径等主要结构参数对涡流管的制冷制热性能的影响。实验中以空气为介质分别对不同结构参数涡流管的性能进行了研究,得出了热端管管长、分离室直径以及冷孔板孔径等参数对涡流管制冷制热性能的影响规律。研究结果表明:在一定范围内增加热端管长度有利于涡流管的能量分离;在大冷流率下,大直径涡流管的制冷性能优于小直径涡流管;冷孔板孔径愈小,涡流管的制冷制热效应都愈好,在冷孔板孔径与热端管内径之比为50%时,取得最佳的制冷制热效应。      

基于并行遗传算法压气机叶片自动优化设计

结合小生境法与算子自适应法对基本遗传算法进行改进,采用WinSock接口、多线程、CS体系结构,实现并行遗传算法.将并行遗传算法与NS方程流场计算方法、Hicks-Henne函数叶型参数化方法结合构成叶型自动优化设计软件,软件可用于叶型设计和对已有叶型的改进.在构造目标函数时,根据工作攻角范围,构造了考虑非设计点性能的目标函数.分别对进口马赫数为0.5和0.9左右的叶栅采用三台计算机进行并行气动优化设计,优化叶型设计点和非设点性能都明显好于原始叶型.     

压气机进口档板动态畸变流场参数分析

对某型发动机压气机进口档板动态畸变流场数据进行了研究。分析了流场稳态总压、总压脉动强度和涡旋尺度随档板插入深度、压气机流量的变化规律,以及各动态参数之间的相对变化特点;初步探讨了涡旋尺度、总压脉动强度、综合畸变指数和压气机喘振裕度损失等性能参数变化的关系,获得了有价值的试验研究数据结果。     

非结构动网格技术及其在超声速飞行器头罩分离模拟中的应用

针对激波诱导物体运动的二维动力学模型,比较了采用流动定常、结合非定常弹道方程的所谓"准定常"计算方法和非结构动网格计算方法,通过流场和运动特性分析,指出发展有相对运动的非定常流动模拟方法的重要性;另外采用修正弹簧近似和局部重构的非结构动网格技术,耦合求解Euler方程及6DOF弹道方程,数值模拟高度H=25km、飞行马赫数Ma=6.0、迎角α=0°状态下火箭抛罩的动力学过程.研究表明,稠密大气层内头罩受到的气动力比惯性力大几个数量级,导致头罩的运动特性完全由气动力控制.分离过程中,头罩和火箭头部之间的气动干扰在时间和空间上都表现出强烈的非线性特征,头罩姿态变化剧烈.本文还对分离过程中部分位置上的流场进行定常模拟,比较了定常和非定常的气动力,所得结论对于分析地面风洞可控轨迹系统(CTS)试验具有指导意义.     

基于Nash-Pareto策略的两种改进算法及其应用

针对多目标、多设计变量的优化问题,提出了两种优化的新算法:一种是将多目标问题转化为单目标时,对目标权重的确定提出了新的途径;另一种是直接对多目标问题进行优化,并对Pareto遗传优化技术作了改进,以得到均匀分布的Pareto最优解集.两种新算法都是建立在Nash的系统分解与Pareto遗传算法的基础上,因此称这类算法为Nash-Pareto策略.借助于这类算法,文中以跨声速压气机双圆弧类叶型的气动优化为例,给出了气动优化的全过程.数值优化的实验表明所给出的改进算法是可行的、有效的.     

双肋式微型气动阀的数值计算与实验

 针对现有微型三角阀效率低的问题,提出双肋式气动阀这一新型微阀,通过两级带圆弧过渡的收敛形肋条,在减小正向气流压力损失的同时,引导逆向气流分为3股后再呈“Y”形汇聚,产生强烈的相互撞击而抵消部分动能,从而减小逆向流量以提高效率。通过数值计算对双肋式气动阀的作用原理进行了分析与验证;加工了特征尺寸为1 mm的三角阀、梯形阀与双肋阀实验件,并设计了相应的实验方案,在微流体实验平台上进行了对比实验。结果表明双肋阀能大幅提高效率：对不可压流,双肋阀可将效率从普通阀的2%～3%提升至14%左右;对可压流,双肋阀能将效率从2%提升至约13%。     

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.