面向图形对象技术在风洞应变天平CAD系统中的应用

ARX是新一代面向对象的AutoCAD开发环境，在介绍其特征和功能的基础上，对风洞应变天平CAD系统开发中的一些关键技术进行了讨论，介绍了系统的总体结构，数据库的建立、阻力优化设计的数学模型和应用MFC实现图形用户化界面的设计思想与实现技术。ARX支持面向对象技术的特性改变了传统CAD软件的开发模,显示了广阔的应用前景。     

高速风洞超大迎角试验技术初步研究

大迎角风洞试验技术是先进高机动飞行器研制必需的关键技术。气动中心发展的高速风洞超大迎角试验技术 ,包括大迎角机构、模型、天平等。 1 .2m风洞超大迎角试验结果与 2 .4m量级的大风洞试验数据具有较好的一致性 ,试验精度基本达到了××标准对小迎角试验精度的要求 ,表明 1 .2m风洞超大迎角试验技术研究获得了成功。     

NACA0012翼型跨音速测压实验研究

本文为NACA0012翼型在NH-1风洞进行跨音速二维测压实验的研究报告。文中将本风洞的实验结果与国外大风洞的相应实验结果及国内某些理论计算结果作了比较。比较表明曲线规律一致,数据符合较好,说明按现行实验方法得到的本风洞跨音速测压数据是可靠的。本文还对参考点M数、洞壁干扰修正及激波位置等问题作了简要的分析。     

颤振主动抑制中的非线性问题

本文采用谐波平衡法,定量地解释了机翼颤振主动抑制风洞试验中出现的极限环现象。提出了比较精确的计及极限环基阶谐波与三阶谐波的分析计算方法。指出在采用液压舵机的情况下,伺服阀的不灵敏区是出现极限环现象的一个主要原因。     

定/变热线过热比跨超声速流场湍流度测量

开展了基于定、变热线过热比方法测量跨超声速流场湍流度的比较研究,以满足高速飞行器与发动机的跨超声速风洞高精度实验需求。在1.2 m暂冲式跨超声速风洞上,采用定过热比、变二过热比和变八过热比等三种热线测量方法,完成了马赫数为0.30~4.25的跨超声速流场湍流度测量研究。测量结果表明：变八过热比测量精度最高,实测湍流度的蒙特卡洛模拟不确定度为0.001%~0.033%;定过热比方法与变二过热比方法可实现更快速的测量,在马赫数为0.40~2.00范围内与变八过热比测量湍流度均值偏差约9%~18%。研究结果对跨超声速流场湍流度校测、飞行器实验鉴定和数值计算具有实际助益。     

防风工程对风特性及铁道车辆横风气动特性的影响

本文以现场实测和风洞及水槽模拟实验结果为依据,论述了不同类型不同高度的挡风墙及铁路路堤对大风特性和车辆横风气动特性的诸多影响。     

Interplanetary scintillation observations of the high-latitude solar wind

Until the ULYSSES spacecraft reached the polar regions of the solar wind, the only high-latitude measurements available were from indirect techniques. The most productive observations in regions of the solar wind between 5R and 200R have been the family of radio scattering techniques loosely referred to as Interplanetary Scintillation (IPS) (Coles, 1978). Useful observations can be obtained using a variety of radio sources, for example spacecraft beacons, planetary radar echoes and compact cosmic sources (quasars, active galactic nuclei, pulsars, galactic masers, etc.). However for measurement of the high-latitude solar wind cosmic sources provide the widest coverage and this review will be confined to such observations. IPS observations played a very important role in establishing that polar coronal holes (first observed in soft x-ray emission) were sources of fast solar wind streams which occasionally extend down to the equatorial region and are observed by spacecraft. Here I will review the IPS technique and show the variation of both the velocity and the turbulence level with latitude over the last solar cycle. I will also outline recent work and discuss comparisons that we hope to make between IPS and ULYSSES observations.     

子午面太阳风结构及其对日冕抛射物运动的影响

本文提出了一种求解二维理想磁流体力学方程组的组合格式-网格方法。该方法在保证一定精度的前提下稳定性好,计算量小。文中使用该方法算得了子午面太阳风的盔状流动解。以该解作为初态,研究了盔状冕旒位形对日冕抛射物运动的影响,发现该位形使得抛射物向低纬赤道方向偏转,较好地解释了观测结果。     

日地共转扰动似稳结构及其反相和漂移规律的最新证据

日地共转扰动似稳结构及其反相现象在第２１及２２周再次显现，从而证实了上述发现是一种在长达世记的时间尺度内存在的普遍规律。包括１９９１－１９９２年内的百年地磁扰动资料还说明偶数太阳周的共转似稳结构扰动峰有逆太阳自转而线性性漂移的趋向。对即将来临的极小年前可能出现的共转扰动作了试验性的预测。     

On the correlation of the solar wind observed at the L5 point and at the Earth

The L5 point is a promising location for forecasting co-rotating high-speed streams in the solar wind arriving at the Earth. We correlated the solar wind data obtained by the Nozomi spacecraft in interplanetary space and by the Advanced Composition Explorer (ACE) at the L1 point, and found that the correlation is significantly improved from that of the 27-day recurrence of ACE data. Based on the correlation between the two spacecraft observations, we estimated the correlation of the solar wind velocity between the L5 point and at the Earth, and found that the correlation coefficient was about 0.78 in late 1999, while that of the 27-day recurrence was 0.51. Eighty-eight percent of the velocity difference falls within 100 km/s between the L5 point and the Earth. This demonstrates the potential capability of solar wind monitoring at the L5 point to forecast the geomagnetic disturbances 4.5 days in advance.