扇翼气动特性试验研究

通过对扇翼飞行器采用风洞试验的方法,研究横流风扇在不同风扇转速、来流速度、迎角、前缘开口角和叶片安装角下的升力、阻力和需用功率,得到相关的试验数据,并进行了处理分析。结果表明:风扇转速是影响扇翼升推力的主要因素,不同迎角和来流速度下扇翼的气动特性也不相同,前缘开口角和叶片安装角对扇翼的气动特性影响也比较大。本试验进一步验证了扇翼的工作原理以及获得控制扇翼飞行器升推力的方法,为大尺寸扇翼无人机的设计制作提供技术支撑。     

0.8m 风洞风扇系统的设计和运转

为提高低速风洞的最大风速,根本的措施是设计高转速大功率的风扇系统。风扇系统的设计首先在于有一个良好的设计方法,选择高升阻比的风扇翼型,根据需要恰当地确定设计工况点,合理选择桨叶和反扭导流片的各个参数,如桨毂比、实度、升力系数和圆弧角等。设计中针对已经设计的外形,进行性能计算,可以迅速鉴别设计的优劣,检查是否能满足设计要求,节约研制成本和缩短周期。     

基于VXI总线的高速风洞脉动压力测试与分析系统

VXI总线代表着当今自动测试领域的发展方向。笔者介绍了气动中心高速所组建的基于VXI总线的高速风洞脉动压力测试系统,文中给出了测试仪器的计量指标,并简要说明了测量与分析软件的开发过程。通过风洞试验的实际检验,表明该套系统性能先进,稳定可靠,具有广泛的应用前景     

新型空气低温跨声速原理性风洞研制

为解决常规风洞雷诺数模拟不足的问题,采用低温风洞已被证明是一条可行的途径。目前世界上几乎所有运转的低温风洞都是采用液氮气化吸热方法来降低和保持试验气体的温度。对于大型低温风洞,这种制冷方案存在着运转费用高昂和环境污染的缺点。为克服上述缺点,俞鸿儒院士提出了一种用空气作试验气体,藉热分离器制冷并回收排气冷量的新型低温风洞的概念。此原理性风洞的研制就是要从其基本原理、设计特点及实验结果等方面来验证和探讨这种新概念的可行性和应用前景。     

大型双曲冷却塔表面脉动风压随机特性——风压极值探讨

针对风压信号呈现的非高斯特性和传统极限估计方法的局限,首次提出基于保证率和相关性的极值估计方法——全概率迭代法进行冷却塔表面脉动风荷载极值分析,并和传统的峰值因子法及改进的Sadek-Simiu法计算结果进行对比验证。结果表明：全概率迭代法避开了对随机过程的高斯分布假定,相比传统的极值估计方法其结果更加真实可靠;表达风压极值中脉动分量的峰值因子数值沿着环向和子午向变化显著,如取为同一数值则偏于危险或过于保守;采用全概率迭代法得到的表面风压系数极值分布曲线与规范取值相比,迎风面和负压峰值区域极值偏小,背风区域极值偏大,且最小值对应角度相差约10°。     

Geomagnetic activity driven by solar wind turbulence

Within the framework of the solar wind—magnetosphere coupled system, intense perturbations in the solar wind, causing geomagnetic storms and substorms, have been widely studied by means of the so-called coupling parameters. However, remarkable variations in the geomagnetic field occur even in absence of such perturbations. In those conditions, solar wind MHD turbulence might have a role. Recent results have shown that solar wind turbulence can be described not only as a mixture of inward and outward stochastic Alfvénic fluctuations, but includes also advected structures, dominated by an excess of magnetic energy.     

The effects of the solar magnetic polarity and the solar wind velocity on Bz-component of the interplanetary magnetic field

We have studied the effect of both solar magnetic polarity and the solar wind velocity on the Bz-component of the interplanetary magnetic field, IMFBz, for the minimum activity of the solar cycles 21, 22, 23 and 24. We made a statistical study of IMFBz in the first section which is considered as an extension of Lyatsky et al. (2003). They made a statistical study of IMFBz for two periods of minimum solar activity 22 and 23 related to 1985–1987 and 1995–1997 when the solar magnetic field had opposite polarity. Our results seem to be consistent with the results obtained by Lyatsky et al. (2003). We found that there is a dependence of IMFBz on the IMFBx and the solar magnetic polarity for the minimum periods of the selected four solar cycles. In addition, we found that there is a dependence of IMFBz on the solar wind velocity.     

水气动量交换的实验研究

在风浪槽中进行水气动量交换实验，测量了不同风速和风区下的波浪及空气湍流流场。测量数据表明水面上风速分布符合对数律，水气界面附近在小范围的动量交换常通量层。阻力系数ＣＤ随风速增加线性增长，随波龄增加而减小。这一趋向与理论分析及外海帝测结果一致。对风浪发展过程中波浪和空气湍流谱结构的分析证明了水气运动的耦合关系。     

椭球台高杆灯风荷载的实验研究

通过风洞实验研究了多钝体高杆灯在不同水平风向角和竖向风向角下的力与力矩系数。实验结果表明在一定的风向角下，法向阻力系数Cdmax=1.030,法向弯曲力矩系数Cmmax=-0.940,轴向力系数Camax=0.504和Camin=-0．600。     

Solar cycle variation of “killer” electrons at geosynchronous orbit and electron flux correlation with the solar wind parameters and ULF waves intensity

To construct models for hazard prediction from radiation belt particles to satellite electronics, one should know temporal behavior of the particle fluxes. We analyzed 11-year variation in relativistic electron flux (E>2 MeV) at geosynchronous orbit using measurements made by GOES satellites during the 23rd sunspot cycle. As it is believed that electron flux enhancements are connected with the high-speed solar wind streams and ULF or/and VLF activity in the magnetosphere, we studied also solar cycle changes in rank order cross-correlation of the outer radiation belt electron flux with the solar wind speed and both interplanetary and on-ground wave intensity. Data from magnetometers and plasma sensors onboard the spacecraft ACE and WIND, as well as magnetic measurements at two mid-latitude diametrically opposite INTERMAGNET observatories were used. Results obtained show that average value of relativistic electron flux at the decay and minimum phases of solar activity is one order higher than the flux during maximum sunspot activity. Of all solar wind parameters, only solar wind speed variation has significant correlation with changes in relativistic electron flux, taking the lead over the latter by 2 days. Variations in ULF amplitude advance changes in electron flux by 3 days. Results of the above study may be of interest for model makers developing forecast algorithms.