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.     

地源热泵技术在建筑节能中的应用

本文探讨如何通过地源热泵技术实现建筑节能。研究通过地源热泵来实现一机多用,使其既能用于冬季供暖,又可以用于夏季制冷。同时也讨论了如何与太阳能相配合,来实现地热平衡。文中还给出了通过插值法和曲线拟合法对测量数据进行处理获得变温带和增温带的温度-深度曲线的方法。     

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。     

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。     

飞翼模型高速风洞PIV试验研究

对小展弦比飞翼标模在2.4米跨声速风洞中创新开展了PIV试验。对空风洞进行了测速校核,并对小展弦比飞翼标模开展了二维、三维涡迹PIV测试,试验马赫数为0.4~0.9。测试结果表明,2.4m风洞PIV试验数据具有较高的准确度,M≤0.8时空风洞测速结果与理论值相差不超过1%,M=0.9时相差不超过2%。小展弦比飞翼标模测试结果显示,M数增大使机翼尾涡涡量和切向速度增大,涡核向内展向方向移动。前缘涡与上翼面分离具有密切关系:当M=0.8、α≤12°时,翼梢测试截面的前缘涡尚未破裂,上翼面未发生显著的流动分离;当α≥13°时,前缘涡破碎时机提前,当地后1/2弦长区域产生了比较明显的流动分离。     

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。     

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.