侧面突扩燃烧室冷态流场可视化研究

燃烧室流场中旋涡的不是稳定是造成整体式压式发动机侧面扩燃烧室燃烧振荡的重要原因。在透明矩形侧面突扩燃烧室模型上进行了水流模拟显示实验。显示出了燃烧室流场中的振荡涡系和稳定涡系。实验发现：燃烧室头部旋涡非常稳定；进口射流剪切层存在“马蹄涡”的周期性脱落；射流在燃烧室通道内卷绕形成涡强较大的二次流螺旋柱状涡对，涡对相撞又使螺旋涡失稳、振荡和破碎。旋涡不稳定性是侧面突扩燃烧室燃烧振荡的流体力学原因，分流     

圆管内不可压粘流的分布式并行算法

用并行算法求解了圆柱通道内不可压层流流动。采用有重叠的条形区域分裂法时计算域进行分区，分别求解动量方程和压力校正方程，对压力校正方程采用块修正法来加速线代数方程的收敛速度。计算结果表明有较好的并行加速比和并行效率。     

长期贮存的固体火箭发动机药柱的温度应力分析

分析了固体火箭发动机药柱在长期贮存过程中，由于温度载荷谱的变化所引起的力学响应，基于粘弹性积分蠕变型本构关系，推导出了能分析粘弹结构热载荷的有限元模型，并用它分析了梁、厚壁圆筒与真实固体火箭发动机的热应力问题。     

Synergism of binocular and motion stereo for passive ranging

Range measurements to objects in the world relative to mobile platforms such as ground or air vehicles are critical for visually aided navigation and obstacle detection/avoidance. An approach is presented that consists of a synergistic combination of two types of passive ranging method: binocular stereo and motion stereo. We show a new way to model the errors in binocular and motion stereo in conjunction with an inertial navigation system (INS) and derive the appropriate Kalman filter to refine the estimates from these two stereo ranging techniques. We present results using laboratory images that show that refined estimates can be optimally combined to give range values which are more accurate than any one of the individual estimates from binocular and motion stereo. By incorporating a blending filter, the approach has the potential of providing accurate, dense range measurements for all the pixels in the field of view (FOV)     

固体发动机试车燃气中HCl和Al2O3扩散研究

对固体火箭发动机试车燃气的组成，抬升和扩散，采用高斯模式与环境监测相结合的方式进行了系统研究，评价了不同大气稳定度下ＨＣｌ和Ａｌ２Ｏ３浓度的分布，提出了有效的防治措施。     

螺桨气动性能的试验研究

介绍了我国第一次进行的螺桨风洞试验-某型螺桨模型及改型桨模型风洞对比试验。首次得到了系统的缩尺模型性能对比试验结果。试验表明改型桨在爬升、巡航效率、静拉力等方面均超过设计要求的指标。介绍了螺桨驱动装置、试验模型、测量系统、试验修正、结果分析等。      

IMF connection for energetic protons observed at Ulysses via mid-latitude solar wind rarefaction regions

As Ulysses moved inward and southward from mid-1992 to early 1994 we noticed the occasional occurrence of inter-events, lasting about 10 days and falling between the recurrent events, observed at proton energies of 0.48–97 MeV, associated with Corotating Interaction Regions (CIR). These inter-events were present for several sequences of two or more solar rotations at intensity levels around 1% of those of the neighbouring main events. When we compared the Ulysses events with those measured on IMP-8 at 1 AU we saw that the inter-events appeared at Ulysses after the extended emission (>10 days) of large fluxes of solar protons of the same energy that lasted at least one solar rotation at 1 AU. The inter-events fell completely within the rarefaction regions (dv/dt<0) of the recurrent solar wind streams. The interplanetary magnetic field (IMF) lines in the rarefactions map back to the narrow range of longitudes at the Sun which mark the eastern edge of the source region of the high speed stream. Thus the inter-events are propagating at mid-latitudes to Ulysses along field lines free from stream-stream interactions. They are seen in the 0.39–1.28 MeV/nucleon He, which exhibit a faster decay, but almost never in the 38–53 keV electrons. We show that the inter-events are unlikely to be accelerated by reverse shocks associated with the CIRs and that they are more likely to be accelerated by sequences of solar events and transported along the IMF in the rarefactions of the solar wind streams.     

Ulysses observations of a coronal origin particle event at 32° south heliographic latitutde

A remarkable streaming beam-like particle event of 60 keV-5 MeV ions and of 38–315 keV electrons has been reported previously. This event has been associated with the passage of a Coronal Mass Ejection (CME) over the Ulysses spacecraft on June 9–13, 1993. At this time, the spacecraft was located at 4.6 AU from the sun and at an heliolatitude of 32° south. It was proposed (Armstrong et al., 1994) that the particle injection source could have been of coronal origin. In this study, we analyse the solar activity during this period. We identify a region of solar radio noise storms in the corona and in particular, a flare on June 7 that presents all the required characteristics to produce the hot plasma beam observed in the interplanetary medium.     

Pioneer and Voyager observations of large-scale spatial and temporal variations in the solar wind

The Pioneer 10, Pioneer 11, and Voyager 2 spacecraft were launched in 1972, 1974, and 1977, respectively. While these three spacecraft are all at compartively low heliographic latitudes compared with Ulysses, their observation span almost two solar cycles, a range of heliocentric distances from 1 to 57 AU, and provide a unique insight into the long-term variability of the global structure of the solar wind. We examine the spatial and temporal variation of average solar wind parameters and fluxes. Our obsevations suggest that the global structure of the outer heliosphere during the declining phase of the solar cycle at heliographic latitudes up to 17.5°N was charaterized by two competing phenomena: 1) a large-scale increase of solar wind density, temperature, mass flux, dynamic pressure, kinetic energy flux, and thermal enery flux with heliographic latitude, similar to the large-scale latitudinal gradient of velocity seen in IPS observations, 2) a small-scale decrease in velocity and temperature, and increase in density near the heliospheric current sheet, which is associated with a band of low speed, low temperature, and high density solar wind similar to that observed in the inner heliosphere.     

Variations of the high energy electron flux along the Ulysses trajectory

We describe for the first time the analysis of high energy electrons (above 240 MeV) from the COSPIN/KET experiment onboard Ulysses. The electron time profiles in four energy windows are presented from Oct. 90 to the end of March 94, up to a maximum heliographic latitude of 57 °S. The recovery rates we derived for the electrons are compared to the recovery rates of positively charged particles with the same rigidity.