雷达有源诱偏与反辐射导弹对抗仿真技术

简要分析反辐射对抗技术的发展应用情况,分析并提出了雷达有源诱偏与反辐射导弹对抗性能评估试验方法,最后介绍了一种抗反辐射导弹有源诱偏路馈半实物仿真系统研制与试验情况。     

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。     

翼板颤振主动抑制的无限维非线性分析

 <正> 1.混合动力学系统的Hopf分叉定理 本文将Marsden-McCracken关于分布参数的Hopf分叉定理推广至混合动力学系统。 设在积空间X=E×R~n中依赖参数μ的演化方程为     

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。     

机翼/外挂系统的颤振主动抑制研究

 本文对颤振主动抑制控制律进行了研究。研究对象为一小展弦比带外侧导弹的机翼颤振模型,模型具有外侧后缘控制面。依据该模型的全部动力特性和刚度特性,以最优控制为基础,采用动态补偿器方法,设计了两阶控制律。对该控制律进行了风洞实验验证。实验结果表明:颤振临界速度提高了14％以上。理论计算结果与实验结果一致。     

智能旋翼的频域神经控制

 频域内的神经控制方法在振动主动控制中因其允许复杂的控制算法,适合于智能旋翼的控制。在建立频域智能旋翼系统模型的基础上,提出了频域内的智能旋翼神经控制方法。采用正交设计方法选取训练样本,建立频域神经模拟器,然后按照提出的算法进行控制。仿真结果表明提出的算法有效,并且具有较好的鲁棒性。     

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.