直接的矩阵分裂计算跨音速喷管流场

给出了分离系数矩阵求解欧拉方程组时系数矩阵的直接分离公式，减少和简化了应用该方法时的矩阵运算，参照Ｂｅａｍ－Ｗａｒｍｉｎｇ显式格式构造与ＳＣＭ方法一致的内点差分格式，并分析了它的数值特性，对有斜激波的跨音速内流场进行了数值仿真。计算中采用变系数的当地时间步长，加快了流场达到的收敛速度，计算无需引入任何人工参数，计算值与实验结果吻合。     

T／R－R型双基地系统分段跟踪技术的研究

根据Ｔ／Ｒ－Ｒ型双基地系统在受到由弱到强的干扰影响时,其可用的测量量不同,有必要研究各种干扰模式下应采用的跟踪算法,提出了分段跟踪技术,充分利用了不同干扰强度时Ｔ／Ｒ站和Ｒ站的测量数据,提高了对三维运动目标的跟踪精度。通过典型目标航迹的计算机仿真,对算法性能做了评估。     

The Freja wave and plasma density experiment

The Wave Experiment, F4, on the Swedish/German satelliteFreja, is designed to measure the electric wave fields up to 4 MHz, the magnetic wave fields up to 16 kHz and the plasma density and its relative variations up to 2 kHz. Six wave signals and four density probe signals can be measured simultaneously. The wave forms of all signals are transmitted to ground without any analysis onboard. The limited TM allocation does not allow continuous sampling of the wave signals, so normally the measurements are made in snapshots of various lengths dependent on sampling frequency, etc. Continuous sampling can be made for shorter time periods by using a 6 Mbyte memory as a buffer.     

Broadening of Fe X (6374 Å) profiles above the limb in a coronal hole

Profiles of the visible Fe X (6374 Å) coronal emission line as a function of height above the limb were obtained out to 1.16 solar radii in a coronal hole using the NSO/Sacramento Peak Observatory Coronagraph, Universal Spectrograph and a CCD camera. These are the first coronal line profiles obtained as a function of height in a coronal hole from the ground. Analysis of the line widths suggests a large component of nonthermal broadening which increases with height ranging from 40 to 60 km/s, depending upon the assumed temperature or thermal component of the profile.     

二级入轨航天运载器最优分离飞行状态研究

研究水平起降二级入轨航天运载器分离飞行状态（飞行高度、轨迹倾角、马赫数）对轨道器在分离点处的质量（包括结构质量、燃料质量等）的影响。主要内容包括：针对以火箭发动机为动力的轨道器，建立了上升段运动方程。采用静态可变误差多面体算法加上动态共轭梯度法数值优化了轨道器上升段轨迹，优化的性能指标是分离点处轨道器的总质量最小，初始条件受到载机上升段走廊的约束，终端约束是某指定的目标轨道。对分离状态与轨道器总体方案（升阻比、推力、比冲等）对轨道器总质量的影响作了大量数值仿真。针对某飞行器模型，得到了一组最优分离飞行状态。拟合出估算分离状态对轨道器总体方案的影响计算公式。得到了合理选择分离飞行状态的结论。     

弧齿锥齿轮波动共振条件分析

应用弹性理论和波动理论, 推出旋转盘形弧齿锥齿轮波动响应的模态解, 重点讨论了啮合力F对齿轮波动共振的影响。给出了弧齿锥齿轮波动共振的条件。      

伪距解除相关法在GPS/SINS紧组合系统中的应用研究

介绍了伪距解除相关法的原理 ,设计了一种加权平均跟踪误差估计器 ,用以估计 GPS接收机码环跟踪误差。研究结果表明 ,与未对伪距测量值进行修正时相比 ,应用伪距解除相关技术可以减小组合系统的导航误差 ,提高系统的导航精度     

轴对称件超塑约束胀形过程FEM模拟

采用大变形刚粘塑性有限元 ( FEM)模拟了圆板轴对称超塑约束胀形的贴模过程。研究了胀形件几何尺寸 (胀形高宽比 HP/RD)、材料速率敏感指数 m、摩擦因子 Am 对胀形件贴模过程 ,以及贴模方式对厚度不均的影响     

涡喷发动机压气机的单元控制体模型

根据控制体理论,建立了涡喷发动机中压气机的逐级数学模型。采用特征线关系数值求解质量、动量和能量方程。方程中的叶片力和轴功由稳态的级特性提供,并由一阶滞后方程考虑其动态效应。该模型可以模拟进口温度（或压力）瞬变下压气机的逐级响应,寻找首先失速的关键级。数值结果表明,引起失速的进口温升近似地与进口温升率呈线性关系。     

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.