自然风条件下露天试车台推力修正的数值模拟研究

为研究航空发动机在露天试车台的推力修正方案,开展航空发动机在不同自然风风速(0到5m/s)、风向(0到90°)下露天试车的数值仿真计算。分析不同自然风条件露天试车发动机进气道周围和进气道气动交界面流场分布特点,发现已往基于测量二次气流的室内试车台推力修正方法无法用于露天试车台;通过内流法推导出适用于露天试车台的航空发动机进气附加阻力计算公式,在此基础上结合仿真结果计算露天试车台发动机进气附加阻力和台架迎风阻力,并分析的风速对各项修正阻力的影响规律,给出台架迎风阻力与环境风速之间的拟合关系式,研究不同风向的侧风对台架阻力的影响规律。研究结果为实际露天基准试车试验开展提供理论研究帮助,并为测量推力修正给予指导。     

捕获加速新生离子对Alfvén波的激发

根据准线性方程,求出了在离子持续产生并被太阳风捕获加速的情况下离子的渐近态分布函数.采用此分布函数分析了斜向传播的Alfven波的稳定性.     

宁静和重现太阳风中的亚阿尔文波速流

本文例举观测实例说明,在宁静太阳风中或重现太阳风的低速流区,有可能形成行星际亚阿尔文波速流。这种流出现在阿尔文波速异常增强区,并与特定的磁场位形相联系。      

根据行星际闪烁(IPS)的双频互谱估计太阳风速度

本文讨论了观测频率为232MHz和327MHz时,利用互谱的方法估计太阳风速度的可能性、考虑路径积分效应,结果表明在17°≤ε≤50°范围内,对于几种可能的太阳风速度分布,由互谱所得结果与太阳风速度值差别小于15%.      

Sharp boundaries of solar wind plasma structures and their relationship to solar wind turbulence

Sharp (<10 min) and large (>20%) solar wind ion flux changes are common phenomena in turbulent solar wind plasma. These changes are the boundaries of small- and middle-scale solar wind plasma structures which can have a significant influence on Earth’s magnetosphere. These solar wind ion flux changes are typically accompanied by only a small change in the bulk solar wind velocity, hence, the flux changes are driven mainly by plasma density variations. We show that these events occur more frequently in high-density solar wind. A characteristic of solar wind turbulence, intermittency, is determined for time periods with and without these flux changes. The probability distribution functions (PDF) of solar wind ion flux variations for different time scales are calculated for each of these periods and compared. For large time scales, the PDFs are Gaussian for both data sets. For small time scales, the PDFs from both data set are more flat than Gaussian, but the degree of flatness is much larger for the data near the sharp flux change boundaries.     

单流体二维太阳风结构的磁流体力学模拟

在添加动量项的条件下，对单流体二维磁流体力学方程组进行模拟，得到了子午面上的太阳风结构，结果表明，添加动量项的形式及其被加入的位置对远区太阳风速度和质子密度有重要的影响。本文在适当的区域加入合适的动量项得出了远区太阳风速和质子密度与Ulysses观测基本符合的结果。文中给出了较合适的动量添加区域为3.5-10Rs(Rs为太阳半径）。     

A Revisit of the Phobos Events

The magnetic field disturbances detected by the Phobos-2 spacecraft in 1989 have been suggested to be caused by a ring of dust and/or gas emitted from the Martian moon, Phobos. The physical nature of these ``Phobos events' is examined using results from related investigations over the last twenty years. It is concluded that there is no clear evidence at present to support the association of magnetic field disturbances in the solar wind with Phobos. The situation will be further clarified taking advantage of the multi-spacecraft observations of the Yinghuo-1(YH-1), Mars Express and MAVEN missions beginning in 2012. It is expected that many novel features of solar wind interaction with Phobos (and possibly also Deimos) itself will also be revealed.      

Spatial variation of the supersonic thermal plasma flow downstream of the termination shock

In this paper we start from the most recently observed fact that the solar wind plasma after passage over the termination shock is still supersonic with a Mach number of about 2. To explain this unexpected phenomenon and to predict the evolution of properties of the downstream plasma flow we here consider a two-fluid proton plasma with pick-up protons as a separate suprathermal, second proton fluid. We then formulate a self-consistent system of hydrodynamical conservation equations coupling the two fluids by dynamical and thermodynamical coupling terms and taking into account the effects of newly incorporated protons due to charge exchange with the H-atoms in the heliosheath. This then allows us to predict that in the most probable case the solar wind protons will become subsonic over a distance of about 30 AU downstream of the shock. As we can also show, it may, however, happen that the plasma mixture later again reconverts to a supersonic signature and has to undergo a second shock before meeting the heliopause.     

太阳宁静区磁漏斗结构的扩展特征

通过对观测的光球纵向磁场进行势场外推, 重构了一个太阳宁静区光球以上的磁场结构. 结果显示, 在20 Mm 以下, 开放磁力线呈现多个明显的小磁漏斗结构, 这些小磁漏斗结构随高度扩展, 并且在20 Mm 左右融合成大的漏斗结构. 通过系统地研究磁漏斗结构横截面积随高度的变化趋势, 发现太阳宁静区磁漏斗结构的截面积随高度近似线性扩展, 磁漏斗结构在较低高度上(<20Mm) 扩展的速度比在较高高度上 (>20Mm) 扩展的速度要快. 这一结果对太阳风起源和磁环中物质流动的二维数值模拟具有重要的意义. 同时还发现, 闭合磁力线的数目随高度以指数函数的形式减少.      

基于单应性矩阵的模型迎角单目视频测量方法

风洞试验中模型迎角的精准测量是降低阻力系数误差的重要途径之一,为此,提出了基于单应性矩阵的模型迎角单目视频测量方法。该方法通过两个单应性矩阵,获取试验过程中相机实时位姿和标记点物方空间位置坐标,应用坐标旋转关系,完成试验模型的迎角测量。数值仿真试验结果表明：迎角测量误差与待测标记点到风洞壁板间的距离偏差近似为线性关系,因此,当标记点不满足共面条件时,可根据该特点进行测量误差修正。静态标定和风洞迎角测量试验结果表明：修正系统误差后,迎角实测数据的测量准度在0.01°以内,精度不超过0.012°。本文方法易于实施,工程实用价值强。