无人机自由编队飞行的补偿模糊神经网络控制

为了克服当前提出的无人机编队飞行的不足，提出一种新的无人机编队飞行概念——自由编队飞行，制定了相关的避让规则，用补偿模糊神经网络进行训练，实现自由编队飞行的补偿模糊神经网络控制。仿真显示，编队飞行的飞机能按照规则自主改变航路进行避让，表明了该方法的有效性。     

用Visual FoxPro进行动态界面的设计

本文介绍用 Visual FoxPro的定时器。标签、按钮等控件和控件的属性、方法、事件等在界面上设计动态字幕、动态按钮等若干动态效果的方法。     

逆合成孔径雷达信号处理方法研究进展

在简要评述国内外现有的逆合成孔径雷达（ISAR）信号处理的运动补偿和成象方法之后，介绍了南京航空航天大学ISAR课题组近年来在ISAR信号处理方法研究中取得的主要进展，包括基于多散射点定位观点的雷达成象观测模型，基于最大似然原理的同时运动补偿和成象方法，基于最大似然原理的多目标成象方法和基于时频分析的多目标成象方法，以及超分辩成象方法，文末指出了在ISAR信号处理方面有待进一步研究的问题。     

非线性条件下编队卫星周期性相对运动条件

利用编队卫星机械能守恒原理，提出了非线性条件下求解编队卫星周期性相对运动条件的新方法，给出了非线性周期相对运动的初始条件。编队卫星相对距离较近时，利用非线性周期运动条件，可修正Hill方程的初始条件，抑制编队卫星的长期漂移。编队卫星相对距离较大，非线性因素不可忽略时，利用非线性周期运动条件，可找到不需消耗任何燃料的周期性相对运动轨道。最后的数值仿真结果验证了该方法的正确性。     

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。     

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.