边界层厚度对腔体气动声学特性影响数值模拟

为了研究来流边界层厚度对开式腔体气动声学特性的影响,基于分离涡模拟方法,计算了来流马赫数为2.0条件下,不同来流边界层厚度与腔体深度比时,长深比为5.88的腔体流动特性,得到了该腔体声压级的频谱特性.计算结果表明:随着来流边界层厚度增加,形成的剪切层稳定性增强,失稳后上下摆动幅度减少,失稳生成的大尺度涡与超声速主流的相互作用减弱,使得大尺度涡发展到腔体后缘时所具有的平动动能和转动动能降低.大尺度涡撞击腔体后缘在腔体内形成的气动噪声的声压级降低,最大减小幅度达7.5dB.同时各阶模态的频率也发生偏移,偏移值在100Hz左右.基于新的假设重新推导了Rossiter公式,明确了经验常数的物理意义,并以此解释了频率偏移现象.      

基于涡流发生器的风洞侧壁附面层控制

为降低风洞侧壁附面层对半模型数据的影响,在前期数值模拟的基础上,研制了一种适用于2.4m跨声速风洞半模型试验段侧壁的梯形涡流发生器,并进行了试验验证.结果表明:加装涡流发生器效果明显,亚声速范围内能够使附面层厚度降低20%~30%,对主气流均匀性影响可忽略;加装后半模型零升阻力系数降低,升力线斜率增大,压力中心向机身移动,体现了明显的附面层减薄效果,证明所研制的涡流发生器可应用于亚声速半模型试验中.      

平箔片楔形高度对气体止推箔片轴承特性影响

针对波箔型气体止推箔片轴承,建立了箔片结构二维薄板模型,并通过有限差分法和有限元法耦合求解可压缩气体Reynolds方程和气膜厚度方程,获得了给定轴承载荷条件下轴承气膜压力分布、气膜厚度分布、平箔片变形量和功率损耗等轴承特性.通过对比楔形高度分别为25,70,100,200,300μm时的轴承特性仿真结果研究了楔形高度对轴承性能的影响.结果表明:降低楔形高度使轴承气膜压力分布更均匀,并降低了平箔片的局部集中载荷.但楔形高度存在一个最佳值,使得达到相同轴承载荷所需的最小气膜厚度最大,并且轴承具有最小功率损耗,提高了轴承的工作效率.该结果为气体止推箔片轴承的结构设计提供的理论参考.      

相变光盘多层膜系结构的最佳光匹配研究

论述了相变光盘最佳膜系结构的设计。采用导纳矩阵法计算膜系的能量反射率，用量优化计算方法编程计算，提出了第二大极值解作为在工艺上可行的实用光盘的膜系结构，并按这种膜系结构制作样品，其擦写循环数达１００万次上。     

斜激波极值规律的边界层影响

采用边界层理论与斜激波/膨胀波精确算法，建立一种结合Eckert参考温度法和Illingworth-Stewartson变换法优势的边界层权重算法，用于研究超声速黏性楔面边界层位移厚度对斜激波极值规律的影响。分别应用层流Navier-Stokes方程和湍流Navier-Stokes方程的CFD解算器对边界层新模型进行了算例精度评估。在来流马赫数为1.2~2.4和楔面角为3°~20°的范围内，压强比的相对误差小于0.1%。计入层流与湍流边界层影响的理论模型研究表明，边界层影响使得最优马赫数增加；对于层流边界层，最优马赫数增量约为0.001 5~0.003 3；对于湍流边界层，最优马赫数增量约为0.002 8~0.006 1。     

水平表面气流剪切作用下的水膜厚度

飞机结冰表面上的液态水受气流吹拂作用会发生向后溢流,从而影响结冰区域范围及防冰系统设计;为了获得水膜流动规律,对水平平板表面上气流剪切驱动的水膜流动进行了实验测量和建模分析。通过水膜流动风洞试验台产生高速气流驱动水膜的流动,使用色散共焦位移计测量同一位置的水膜在不同时刻的厚度变化,结果表明气-液界面由底层薄水膜和多种尺度的波动组成,具有变化速度快随机性强的特点。通过水膜厚度随气流速度及水膜雷诺数的变化规律,发现平均水膜厚度与两者均呈现出单调非线性的依赖关系。基于薄水膜流动理论和平均水膜厚度实验结果,提出了高速气流剪切作用下的气-液波动界面剪切因子计算式,适用于风速17.8~52.2m/s,水膜雷诺数26~128之间的平板水膜流动计算。     

EB-PVD制备箔材的厚度均匀性研究

从真空蒸镀中使用的小平面蒸发源理论出发,针对电子束物理气相沉积中为改善箔材厚度分布所须旋转大基板进行蒸镀的情况,建立了该过程的数学模型;并利用该模型对不同的坩埚位置所沉积的箔材厚度进行了定性分析,从而实现了对坩埚与基板相对位置的优化,使基板上沉积的箔材厚度分布可以达到最均匀的状态.最后通过K值的提出使理论和实际箔材厚度的结果趋于一致,即证明所建立的数学模型是合理的.     

Numerical study on flow fields and aerodynamics of tilt rotor aircraft in conversion mode based on embedded grid and actuator model

A method combining rotor actuator disk model and embedded grid technique is presented in this paper, aimed at predicting the flow fields and aerodynamic characteristics of tilt rotor aircraft in conversion mode more efficiently and effectively. In this method, rotor's influence is considered in terms of the momentum it impacts to the fluid around it; transformation matrixes among different coordinate systems are deduced to extend actuator method's utility to conversion mode flow fields' calculation. Meanwhile, an embedded grid system is designed, in which grids generated around fuselage and actuator disk are regarded as background grid and minor grid respectively, and a new method is presented for ‘donor searching' and ‘hole cutting' during grid assembling. Based on the above methods, flow fields of tilt rotor aircraft in conversion mode are simulated, with threedimensional Navier–Stokes equations discretized by a second-order upwind finite-volume scheme and an implicit lower–upper symmetric Gauss–Seidel(LU-SGS) time-stepping scheme. Numerical results demonstrate that the proposed CFD method is very effective in simulating the conversion mode flow fields of tilt rotor aircraft.     

冲击射流的彩虹纹影实验研究

超声速冲击射流在短距、垂直起降飞行器（S/VTOL）以及火箭发射等方面应用广泛,但是伴随着流场与噪声等诸多方面的问题。要研究这一类问题,必先研究这一类超声速流动的波系结构。文章利用彩虹纹影测量系统,对不同距离不同压比的冲击射流进行实验研究,得到了清晰的彩虹纹影实验结果,细致地呈现了冲击射流的波系结构。基于实验结果,对三种不同结构的冲击射流的波系结构进行了详细分析。发现喷嘴与挡板距离较大时,形成的射流结构与自由射流相似,壁面附近的射流区域不明显。随着距离减小,冲击射流出现壁面冲击区附近射流比较剧烈的现象。距离进一步减小时,出现滞止泡等结构,滞止泡的形状与压比相关。此外,实验表明冲击射流形成的马赫盘大小、形状与来流压比相关。     

The ‘soot line’: Destruction of presolar polycyclic aromatic hydrocarbons in the terrestrial planet-forming region of disks

Interstellar material is highly processed when subjected to the physical conditions that prevail in the inner regions of protoplanetary disks, the potential birthplace of habitable planets. Polycyclic aromatic hydrocarbons (PAHs) are abundant in the interstellar medium, and they have also been observed in the disks around young stars, with evidence for some modification in the latter. Using a chemical model developed for sooting flames, we have investigated the chemical evolution of PAHs in warm (1000–2000 K) and oxygen-rich (C/O < 1) conditions appropriate for the region where habitable planets may eventually form. Our study focuses on (1) delineating the conditions under which PAHs will react and (2) identifying the key reaction pathways and reaction products characterizing this chemical evolution. We find that reactions with H, OH and O are the main pathways for destroying PAHs over disk timescale at temperatures greater than about 1000 K. In the process, high abundances of C₂H₂ persist over long timescales due to the kinetic inhibition of reactions that eventually drive the carbon into CO, CO₂ and CH₄. The thermal destruction of PAHs may thus be the cause of the abundant C₂H₂ that has been observed in disks. We propose that protoplanetary disks have a ‘soot line’, within which PAHs are irreversibly destroyed via thermally-driven reactions. The soot line will play an important role, analogous to that of the ‘snow line’, in the bulk carbon content of meteorites and habitable planets.