二维非定常欧拉方程的摄动解在超声速矩形翼上的应用

本文利用超声速线化理论给出的矩形翼载荷系数解析解作为权函数,对沉浮和俯仰谐振的二维平板翼压强系数进行加权修正,获得矩形翼谐振气动力的近似解,计算结果与线化理论数值结果符合得很好,本方法是超声速和高超声速矩形翼非定常气动力的一种统一和快速的计算方法。     

二元流场强激波与紊流附面层干扰下的气流动态畸变控制实验研究

本文在一定的附面层条件下,研究了二元收-扩通道内强激波 M_(U.B.m)为1.68～1.74下的激波与壁面紊流附面层干扰区内的气流动态畸变控制技术,包括抽气缝槽结构,缝槽位置等对干扰区下游动态畸变的影响,并对通道扩张段出口气流的紊流度分布剖面上典型站的总压信号作功率谱密度、概率密度和压力时间历程作了分析.实验的结果表明,通过对干扰区内激波诱导分离流抽吸,在抽气量为W_(bT)/W_m=2.8～3.5%下,可以很有效地改善干扰区下游气流的动态畸变.     

On the off-ecliptic distributions of anomalous cosmic rays and their relation to the large-scale geometry of the heliospheric shock

The scenario explaining the origin of the anomalous component of cosmic rays (ACR) implies a close relation between these high energy particles and the solar wind termination shock representing their main acceleration region. Consequently, one should expect the ACR distributions in the heliosphere to reflect some information about the structure as well as the large-scale geometry of the shock. We study the influence of a non-spherically symmetric heliospheric shock on the off-ecliptic — i.e. high latitude — ACR distributions using a two-dimensional model including their anisotropic diffusion and drift in the heliospheric magnetic field as well as a solar wind flow dependent on the heliographic latitude. The model calculations are used to investigate the probability of a possible polar elongation of the heliospheric shock from observations of the distributions of the ACR at high latitudes during solar minimum conditions.     

会聚爆轰加速金属粉喷涂的激波管研究

利用一种可在卧式激波管中研究粉末冶金的装置——喷涂管研究了爆轰喷涂金属粉时工作气体配比对金属粉氧化的影响。研究表明,工作气体按化学当量配比时,金属粉只有极少量的氧化物;工作气体为富氧时,大部分金属粉被氧化。为了观察高速粉末的喷涂能力,利用白色瓷砖作为工件来进行喷涂,结果表明:金属粉完全打入瓷砖内,利用喷涂管已能把较难熔的金属粉喷涂在各种材料上。     

差动式激光多普勒技术在冲击校准测试中的应用

本文介绍了利用差动式激光多普勒技术实现高加速冲击校准的原理、方法和实际的光学系统。     

耀斑激波的相互作用

采用一维磁流体力学模型和激波装配法，分析两个相继出现的耀斑激波的相互作用.前导激波下游的稀疏波显著改变后随激波的特性，并在它的下游产生强后向快激波.两耀斑激波汇合后将在下游形成密度比约为1.5的接触间断.     

Radio emissions from the outer heliosphere

For nearly fifteen years the Voyager 1 and 2 spacecraft have been detecting an unusual radio emission in the outer heliosphere in the frequency range from about 2 to 3 kHz, Two major events have been observed, the first in 1983–84 and the second in 1992–93. In both cases the onset of the radio emission occurred about 400 days after a period of intense solar activity, the first in mid-July 1982, and the second in May–June 1991. These two periods of solar activity produced the two deepest cosmic ray Forbush decreases ever observed. Forbush decreases are indicative of a system of strong shocks and associated disturbances propagating outward through the heliosphere. The radio emission is believed to have been produced when this system of shocks and disturbances interacted with one of the outer boundaries of the heliosphere, most likely in the vicinity of the the heliopause. The emission is believed to be generated by the shock-driven Langmuir-wave mode conversion mechanism, which produces radiation at the plasma frequency (f _p ) and at twice the plasma frequency (2f _p ). From the 400-day travel time and the known speed of the shocks, the distance to the interaction region can be computed, and is estimated to be in the range from about 110 to 160 AU.Abbreviations PWS Plasma Wave Subsystem - AU Astronomical Unit - DSN Deep Space Network - NASA National Aeronautics and Space Administration - GMIR Global Merged Interaction Region - MHD Magnetohydrodynamic - CME coronal mass ejection - f _p plasma frequency - R radial distance - AGC automatic gain control     

真实火箭燃气羽流密度场的定量显示

本文采用用激光－莫尔偏折和自动测压系统，清晰地显示出真实火箭燃气射流场在激波处的莫尔条纹漂移，首次定量地给出了一种欠膨胀火箭射流的密度分布结果，该结果与射流理论符合较好。     

火箭燃气冲击流场的激波特性

本文详细论述了火箭发射燃气冲击流场的激波特性，侧重讨论了其在平面和斜面上的马赫结构，并就冲击流场的不同情况提出了切合实际的计算模型。