给定通流部分形状时轴流压气机级性能优化

用一维理论对轴流压气机的初步设计作了进一步研究，导出了轴流压气机基元级的特性关系。建立了在给定通流部分形状时最优化设计的数学模型。得到了解析关系。并通过研究给出了数值算例。所得解析关系具有一定的普适性，并可进一步拓展用于多级轴流压气机优化中。     

微肋薄膜减阻的实验研究

作者根据湍流附面层结构新的解释及非光滑特殊造型表面可以减小流体阻力的事实,作者研制了微肋条减阻薄膜,贴在赛船上参加比赛,获得好成绩[1、2] 。作者在风洞中做了贴及不贴微肋薄膜平板试验对比。结果贴微肋薄膜可减阻约 7%。      

基于BICMOS电流控制型多路输出电源的研制

介绍一种适用于低压、宽范围供电的多路输出DC/DC变换器,在功率电路中使用无损耗箝位电路实现了变压器磁芯的复位,控制电路使用第三代BICOMS电流控制型PWM,简化了电路设计、降低了噪声敏感度,给出了多路输出电源中变压器和耦合电感的工程设计的详细过程,同时分析了多路输出耦合电感对负载交叉调节性能的影响.研制的变换器输入电压范围8V-40VDC,输出5V/3A、±15V/0.5A、 10V/0.5A.     

基于小波变换的非平稳信号趋势项剔除方法

分析了空间飞行器遥测信号处理传统趋势项剔除方法的优势和不足,提出了基于小波变换的非平稳信号趋势项剔除方法。这种方法通过滤波器组将信号分解与重构,实现趋向性信号与零均值平稳随机信号的分离。仿真实验表明,该方法简单、高效,适用于非平稳随机信号的处理,是一种实用的趋势项剔除方法。     

一种涡轮发动机加速控制规律设计的新方法

 提出了一种涡喷、涡扇发动机加速控制规律快速设计的新方法：在发动机稳态特性计算模型的基础上,通过额外增加转子提取功率,使得发动机稳态工作点（线）靠近喘振边界,在同时考虑燃烧室富油熄火边界、涡轮进口总温限制以及压气机喘振裕度限制的条件下,利用适当的控制规律描述形式并结合发动机工程研制中的经验,能够快速而准确地获得涡喷、涡扇发动机加速控制规律。对某型涡喷发动机加速控制规律的改进的计算结果表明,提出的加速控制规律的设计方法准确而有效。     

直升机尾桨/尾梁耦合稳定性分析研究

单桨带尾桨直升机的尾旋翼设计成摆振柔软型后,带来了新的动力学问题:尾桨与尾梁耦合动不稳定性问题。本文简述了它与主旋翼/机体耦合动不稳定问题的差别,主要介绍了尾桨与尾梁耦合动不稳定性问题的分析方法,通过算例分析,为消除这种不稳定性,对一些关键设计参数提出了设计要求。     

利用定子槽口宽度削弱永磁电机电磁噪声研究

着重研究了永磁电机定子槽口宽度对电磁噪声的影响。通过电磁力解析计算得出电磁力与定子槽口宽度的计算关系。利用Ansoft软件对1台电动汽车用永磁电机进行电磁场计算,求解改变定子槽口宽度对电磁力波的影响,并用ANSYS软件对该永磁电机进行不同定子槽口宽度的2D声场计算。进行了试验验证,仿真计算与试验结果基本一致,可为该类电机削弱噪声设计计算提供参考。     

航空发动机吞砂试验标准砂与典型沙粒形貌对比分析

航空发动机工作时吸入沙粒会对发动机造成伤害。针对军标中未规定吞砂试验用砂粒的形貌特征问题,提出砂粒形貌特征的统计表述方法——数字图像获取、砂粒圆度(砂粒图片实际面积与其外接圆面积之比)分析、标尺对比与观察统计、振动转换与跟踪、统计指标比较,选取中国南海(海南)、东海(厦门)、腾格里沙漠和塔克拉玛干沙漠等典型地区的沙粒与美国标准砂的形貌特征进行了对比分析。试验表明:利用标准砂进行航空发动机吞砂试验时发动机的损伤最严重,即按照军标要求采用标准砂进行吞砂试验能够保证发动机具有足够的安全裕度。     

Imaging Plasma Density Structures in the Soft X-Rays Generated by Solar Wind Charge Exchange with Neutrals

Both heliophysics and planetary physics seek to understand the complex nature of the solar wind’s interaction with solar system obstacles like Earth’s magnetosphere, the ionospheres of Venus and Mars, and comets. Studies with this objective are frequently conducted with the help of single or multipoint in situ electromagnetic field and particle observations, guided by the predictions of both local and global numerical simulations, and placed in context by observations from far and extreme ultraviolet (FUV, EUV), hard X-ray, and energetic neutral atom imagers (ENA). Each proposed interaction mechanism (e.g., steady or transient magnetic reconnection, local or global magnetic reconnection, ion pick-up, or the Kelvin-Helmholtz instability) generates diagnostic plasma density structures. The significance of each mechanism to the overall interaction (as measured in terms of atmospheric/ionospheric loss at comets, Venus, and Mars or global magnetospheric/ionospheric convection at Earth) remains to be determined but can be evaluated on the basis of how often the density signatures that it generates are observed as a function of solar wind conditions. This paper reviews efforts to image the diagnostic plasma density structures in the soft (low energy, 0.1–2.0 keV) X-rays produced when high charge state solar wind ions exchange electrons with the exospheric neutrals surrounding solar system obstacles.The introduction notes that theory, local, and global simulations predict the characteristics of plasma boundaries such the bow shock and magnetopause (including location, density gradient, and motion) and regions such as the magnetosheath (including density and width) as a function of location, solar wind conditions, and the particular mechanism operating. In situ measurements confirm the existence of time- and spatial-dependent plasma density structures like the bow shock, magnetosheath, and magnetopause/ionopause at Venus, Mars, comets, and the Earth. However, in situ measurements rarely suffice to determine the global extent of these density structures or their global variation as a function of solar wind conditions, except in the form of empirical studies based on observations from many different times and solar wind conditions. Remote sensing observations provide global information about auroral ovals (FUV and hard X-ray), the terrestrial plasmasphere (EUV), and the terrestrial ring current (ENA). ENA instruments with low energy thresholds (\(\sim1~\mbox{keV}\)) have recently been used to obtain important information concerning the magnetosheaths of Venus, Mars, and the Earth. Recent technological developments make these magnetosheaths valuable potential targets for high-cadence wide-field-of-view soft X-ray imagers.Section 2 describes proposed dayside interaction mechanisms, including reconnection, the Kelvin-Helmholtz instability, and other processes in greater detail with an emphasis on the plasma density structures that they generate. It focuses upon the questions that remain as yet unanswered, such as the significance of each proposed interaction mode, which can be determined from its occurrence pattern as a function of location and solar wind conditions. Section 3 outlines the physics underlying the charge exchange generation of soft X-rays. Section 4 lists the background sources (helium focusing cone, planetary, and cosmic) of soft X-rays from which the charge exchange emissions generated by solar wind exchange must be distinguished. With the help of simulations employing state-of-the-art magnetohydrodynamic models for the solar wind-magnetosphere interaction, models for Earth’s exosphere, and knowledge concerning these background emissions, Sect. 5 demonstrates that boundaries and regions such as the bow shock, magnetosheath, magnetopause, and cusps can readily be identified in images of charge exchange emissions. Section 6 reviews observations by (generally narrow) field of view (FOV) astrophysical telescopes that confirm the presence of these emissions at the intensities predicted by the simulations. Section 7 describes the design of a notional wide FOV “lobster-eye” telescope capable of imaging the global interactions and shows how it might be used to extract information concerning the global interaction of the solar wind with solar system obstacles. The conclusion outlines prospects for missions employing such wide FOV imagers.     

不同来流条件下旋转对气膜冷却的影响

大涡模拟考察了旋转状态来流条件对单孔平板气膜冷却的影响,气膜孔沿流向倾斜30°,气膜出流的雷诺数为2 600,吹风比为0.5,计算了静止和旋转数为0.02时气膜冷却的流动和换热,对比两种主流进口条件下旋转对气膜冷却的影响。计算结果表明：（1）均匀来流条件下,旋转主要使发夹涡结构产生非对称分布,裹挟气膜向高半径方向偏转;（2）充分发展的来流条件下,旋转使来流边界层内产生湍流结构,淹没了射流进入主流时产生的发夹涡,引起更强烈的射流扩散,增大了气膜覆盖范围,降低了气膜冷却效率的峰值;（3）旋转通过改变来流边界层内的湍流结构对气膜冷却的影响更显著。