雷诺数对粗糙表面翼型气动性能的影响

采用Spalart-Allmaras湍流模型研究风力机专用翼型DU00-W-212的气动性能。在雷诺数小范围变化的情况下,应用数值模拟的方法对粗糙翼型和光滑翼型的气动特性进行对比。探讨雷诺数小范围变化对粗糙翼型气动特性的影响,并分析升阻力的变化机理。比较升阻力曲线,发现粗糙度对升力系数影响最大的区域在迎角10°附近。小迎角的情况下,前缘粗糙度会使得翼型的升力系数下降,阻力系数反而上升。在大迎角失速的情况下,粗糙翼型的阻力系数反而小于光滑翼型的阻力系数。为了增加叶片适应恶劣沙尘环境的能力,在叶片设计和翼型排布的过程中应该尽量避开升力系数最大的迎角处。     

风力机组叶片的先进翼型族设计

大型风力机组叶片设计需要专用的翼型族,以满足风力机组运行的环境要求。高升阻比、低粗糙度影响是该翼型族的气动性能特点。为了发展我国具有自主知识产权的风力机专用翼型族,在科技部863项目的支持下,北京航空航天大学联合国内气动研究单位,通过理论分析、数值模拟和风洞试验等技术途径,开发了两个适用于大型风力机组叶片的先进翼型族。理论分析和风洞试验表明,设计结果基本达到了预先设定的气动性能指标。     

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.     

翼型测力天平的研制

为研究翼型结冰状态下的载荷变化规律，对翼型进行测力实验。研制一台三分量翼型测力天平。天平设计的突出难点为设计载荷极不匹配，阻力测量载荷很小。设计时，针对翼型载荷的特点，采用片梁组合方式测量阻力，四柱梁测量法向力及俯仰力矩，并采用有限元方法对结构进行了验证计算。主要介绍天平的设计、校准及应用情况。     

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.     

飞翼布局无人机变形机翼设计与模型验证研究

对飞翼布局无人机变形机翼和变形机翼传动机构进行了设计,根据设计结果制作验证模型进行风洞实验和外场飞行试验,以此研究伸缩段机翼对飞行器机翼整体气动性能的影响。结果表明:采用变形机翼技术,可以通过实时控制机翼的气动外形保持较高的气动效率,提高飞机在巡航状态下的升力和高速飞行状态下的机动性,满足飞机在各种任务剖面的战术性能要求。     

建筑物行人高度风环境风洞试验研究

介绍了建筑物风环境的风洞模拟，行人高度风测量探头的设计、标定和数据处理。采用这种探头，在气动中心低速所４ｍ×３ｍ风洞的长１５ｍ、宽４ｍ、高２．２ｍ风工程试验段进行了比例为１∶３００的建筑群模型的行人高度风环境试验研究，结果说明这座新高层建筑物的落成，对其周围某些位置的行人高度风环境有严重的影响。     

UVCS/SOHO Observations of Spectral Line Profiles in Polar Coronal Holes

Ultraviolet emission line profiles have been measured on 15-29 September 1997 for H I 1216 Å, O VI 1032, 1037 Å and Mg X 625 Å in a polar coronal hole, at heliographic heights ? (in solar radii) between 1.34 and 2.0. Observations of H I 1216 Å and the O VI doublet from January 1997 for ? = 1.5 to 3.0 are provided for comparison. Mg X 625 Å is observed to have a narrow component at ? = 1.34 which accounts for only a small fraction of the observed spectral radiance, and a broad component that exists at all observed heights. The widths of O VI broad components are only slightly larger than those for H I at ? = 1.34, but are significantly larger at ? = 1.5 and much larger for ? > 1.75. In contrast, the Mg X values are less than those of H I up to 1.75 and then increase rapidly up to at least ? = 2.0, but never reach the values of O VI.     

A Parallel Adaptive 3D MHD Scheme for Modeling Coronal and Solar Wind Plasma Flows

A parallel adaptive mesh refinement (AMR) scheme is described for solving the governing equations of ideal magnetohydrodynamics (MHD) in three space dimensions. This solution algorithm makes use of modern finite-volume numerical methodology to provide a combination of high solution accuracy and computational robustness. Efficient and scalable implementations of the method have been developed for massively parallel computer architectures and high performance achieved. Numerical results are discussed for a simplified model of the initiation and evolution of coronal mass ejections (CMEs) in the inner heliosphere. The results demonstrate the potential of this numerical tool for enhancing our understanding of coronal and solar wind plasma processes. This revised version was published online in June 2006 with corrections to the Cover Date.