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.     

“大涡破碎”的紊流减阻实验研究

本文对当今国外曾提出的紊流表面摩擦减阻新概念——“大涡破碎”(LEBU)进行了初步的风洞实验探索。将具有对称流线型剖面的二元小肋,沿垂直于气流的方向安置在平板表面的紊流附面层内某一高度处,收到了不同程度的减阻效果。实验中分别考察了小肋的安置位置L,安置高度H,迎角θ及相对厚度b等参数对减阻效果的不同影响。从紊流附面层涡结构的观点出发,提出紊流的“细化”作用是小肋对平扳减阻的根本原因,并认为改善紊流附面层的速度型是研究紊流减阻的一种手段。实验使用自制的高灵敏度摩擦天平,测得的减阻效果与Ludwieg—Tillman公式的计算结果基本一致。     

水陆两栖飞机内吹式襟翼优化设计

为改善某型水陆两栖飞机的起降性能,提高其抗浪能力,需设计高性能吹气襟翼以满足其性能要求。本文在国内外已有的吹气襟翼研究基础上,结合飞机气动综合优化设计框架及计算流体力学(CFD)的优势,以设计出高气动效率及工程实用性的内吹式襟翼方案作为设计目标,对内吹式襟翼的基本形式、吹气缝道位置及喷缝参数等进行综合优化设计,最终通过风洞试验来验证优化设计方案的有效性。从分析及验证结果来看,通过本优化设计方法所设计的内吹式襟翼,能在使用相同吹气动量系数的条件下,明显推迟襟翼上的气流分离,实现最大升力系数20%左右的提升,显著提升了内吹式襟翼的气动效率,为进一步实现内吹式襟翼的工程应用奠定了基础。     

Long-term changes in indices of geomagnetic activity at the auroral station Sodankylä

Here we compare the traditional analog measure of geomagnetic activity, Ak, with the more recent digital indices of IHV and Ah based on hourly mean data, and their derivatives at the auroral station Sodankylä. By this selection of indices we study the effects of (i) analog vs. digital technique, and (ii) full local-time vs. local night-time coverage on quantifying local geomagnetic activity. We find that all other indices are stronger than Ak during the low-activity cycles 15–16 suggesting an excess of very low scalings in Ak at this time. The full-day indices consistently depict stronger correlation with the interplanetary magnetic field strength, while the night-time indices have higher correlation with solar wind speed. The Ak index correlates better with the digital indices of full-day coverage than with any night-time index. However, Ak depicts somewhat higher activity levels than the digital full-day indices in the declining phase of the solar cycle, indicating that, due to their different sampling rates, the latter indices are less sensitive to high-frequency variations driven by the Alfvén waves in high-speed streams. On the other hand, the night-time indices have an even stronger response to solar wind speed than Ak. The results strongly indicate that at auroral latitudes, geomagnetic indices with different local time coverage reflect different current systems, which, by an appropriate choice of indices, allows studying the century-scale dynamics of these currents separately.     

Effects of sector structure of the interplanetary magnetic field on the upper mesosphere–lower thermosphere dynamics

In this paper we study the influence of the interplanetary magnetic field (IMF) polarity changes caused by the Earth passing through the IMF sector boundary on the dynamic processes taking place in neutral atmosphere within the altitude interval of the upper mesosphere–lower thermosphere (83–101 km). The analysis has revealed the influence of the IMF sector structure on dynamics of the upper mesosphere–lower thermosphere. There has been a significant seasonal variation of the wind reaction to the IMF polarity changes observed. The influence of the IMF polarity changes on neutral atmosphere dynamics within the altitude range of 83–101 km is most pronounced in the zonal component of neural wind when the IMF polarity changes from negative to positive in all the seasons except for spring and when IMF polarity changes from positive to negative – in spring only.