后向台阶层流边界层分离实验研究

本文应用偏振差动式激光测速仪对后向台阶层流边界层分离、再附及发展为湍流边界层的整个过程进行了精细的量测,得到了时均速度、湍流强度等的分布特性。我们发现,在本实验条件下,层流边界层分离后在再附点处为过渡流,进一步发展最后形成湍流边界层。在湍流边界层区域,流速分布遵循对数律,但积分常数比平板湍流边界层中所得值要大。     

锯齿型扰流片对壁面压力分布的影响

在风洞用电子扫描阀进行测压,研究了绕平板扰流片和锯齿扰流片分离流动的壁面压力分布.结果表明平板扰流片和锯齿扰流片均在上游x/h=-6处剪切层开始分离,并再附于下游x/h≈20的位置.锯齿扰流片横向位置的变化对壁面平均压力分布几乎没有影响,但通过锯齿槽流向的压力脉动一般大于通过锯齿尖点流向的脉动.从平均压力分布看,锯齿高度可以增加扰流片阻流效果,采用锯齿扰流片可以减小下游壁面压力的脉动.     

形状误差分离技术的统一理论——同源、统一的各种直线形状误差分离方法评述

在对国内外现行直线形状误差分离技术分析研究的基础上,论述了各种分离方法的特点和相互关系,从原理、测量准确度和工程应用方面着眼,评述了直线形状误差测量与分离的各种主流方法--"频域三点法"、"时域递推三点法"、"二点法"、"混合两点法"、"时域乱序四点法"、"精密三点法"和"最小二乘逐次多点法"等.指出了各种方法的同源性和统一性,评述了它们的应用条件及优缺点,同时讨论了随机误差和传感器调零误差的影响及消除方法.     

TC4钛合金的微动磨损及防护

对Ｔｉ－６Ａｌ－４Ｖ合金在１８℃，１００℃２５０℃下的微动磨损特性及防护工艺进行了研究。表明：该合金微动磨损的主要磨损形式是疲劳脱层，其磨损量随温度升高而下降，高渐微动磨损量与磨损区表面所形成的氧化层的性质及厚度有关。     

离散系统仿真输出数据的统计分析

概括了分析仿真产生的数据的方法，讨论了离散系统仿真输出分析的目的以及应用统计方法的要求，对单变量情形，给出了有关估计来自终态仿真和和稳态仿真参数的技术。对多变量情形，以终态仿真为例，给出了用于分析离散系统的仿真输出的某些多变量统计技术，并提出均值向量的估计方法。     

绕丁坝流动结构实验研究

利用流动显示和片光源技术,对绕丁坝的流动进行了实验研究,以便了解丁坝参数对流态的影响.实验是在水槽中进行的.发现在丁坝的上游会形成马蹄涡,在丁坝的背风面会形成卡门涡.按雷诺Re数的大小可以把绕丁坝的流态分成4种类型:定常单个马蹄涡、非定常单个马蹄涡、非定常双马蹄涡Ⅰ及非定常双马蹄涡Ⅱ.实验表明丁坝的交角及丁坝的个数对丁坝的流态有重要影响.     

建立民航维修专家系统的分析

简要介绍了专家系统的原理及构成.分析了“设计民航维修专家系统”的过程,目前加拿大正着手研制的“先进的维修软件系统”的概况.最后提出专家系统需要解决的关键技术问题及发展情况.     

High Excitation ISM and Gas

An overview is given of ISO results on regions of high excitation ISM and gas, i.e. HII regions, the Galactic Centre and Supernova Remnants. IR emission due to fine-structure lines, molecular hydrogen, silicates, polycyclic aromatic hydrocarbons and dust are summarised, their diagnostic capabilities illustrated and their implications highlighted. Based on observations with ISO, an ESA project with instruments funded by ESA Member States (especially the PI countries: France, Germany, The Netherlands, and the United Kingdom), and with the participation of ISAS and NASA.     

逻辑分析仪部分参数测量结果的不确定度评定

介绍了逻辑分析仪部分参数测量结果的不确定度分析评定方法，评定过程及结论，可应用在对于计量标准进行相应指标的不确定度评定分析上。     

Evolution of the Protosolar Nebula and Formation of the Giant Planets

The formation of planetary systems is intimately tied to the question of the evolution of the gas and solid material in the early nebula. Current models of evolution of circumstellar disks are reviewed here with emphasis on the so-called “alpha models” in which angular momentum is transported outward by turbulent viscosity, parameterized by an dimensionless parameter α. A simple 1D model of protoplanetary disks that includes gas and embedded particles is used to introduce key questions on planetesimal formation. This model includes the aerodynamic properties of solid ice and rock grains to calculate their migration and growth. We show that the evolution of the nebula and migration and growth of its solids proceed on timescales that are generally not much longer than the timescale necessary to fully form the star-disk system from the molecular cloud. Contrary to a widely used approach, planet formation therefore can neither be studied in a static nebula nor in a nebula evolving from an arbitrary initial condition. We propose a simple approach to both account for sedimentation from the molecular cloud onto the disk, disk evolution and migration of solids. Giant planets have key roles in the history of the forming Solar System: they formed relatively early, when a significant amount of hydrogen and helium were still present in the nebula, and have a mass that is a sizable fraction of the disk mass at any given time. Their composition is also of interest because when compared to the solar composition, their enrichment in elements other than hydrogen and helium is a witness of sorting processes that occured in the protosolar nebula. We review likely scenarios capable of explaining both the presence of central dense cores in Jupiter, Saturn, Uranus and Neptune and their global composition. This revised version was published online in August 2006 with corrections to the Cover Date.