纤维增强复合材料圆柱壳的屈曲计算

本文利用各向异性多层扁壳的大挠度方程,探讨了正交各向异性多层圆柱壳,在考虑偶合效应和沿厚度方向剪切变形时的轴压,外压及其联合作用下的稳定性问题.用逆解法,给出正交各向异性多层圆柱壳在薄膜力作用下的临界载荷算式.进行了实例计算,并与国内、外实例的实验值比较,符合得相当好.     

网上考试系统的设计与实现

本文讨论了一种新的考试方法———网上考试 ,并讨论了一种基于B/S系统实现网上考试的思路和设计方法 ,并对实现网上考试系统的部分关键技术进行了分析     

民机数据总线信号综合测试仪

介绍的民机数据总线信号测试仪综合了当前民机上主要采用的ARINC429、ARINC419、CSDB和RS232等数字式航空数据总线规范的接口，具有和这些总线接口设备通讯的能力，可以灵活方便地应用于机载设备检测，装机交联实验当中。     

TiAl合金不同钛铝比层片组织的稳定性

对钛铝比为１．１７４、１．１０５和１．０４１的（ＴｉＡｌ）－２．５Ｖ－１Ｃｒ（ａｔ％）合金层片组织在１３２３Ｋ热暴露中的组织变化进行了观察和分析。发现钛铝比对ＴｉＡｌ合金层片组织的稳定性和失稳分解机理有重要影响，钦铝比适当大于１：１（如１．１０５）的合金可以得到稳定性更好的层片组织。     

基于超声波的复合材料层间剪切强度表征分析

采用数字采样、相关分析、频谱分析等方法,结合部分复合材料层板剪切强度试验,验证材料性能与分析结果的对应性、研究分析参数的选择,为无损表征复合材料剪切强度的可行性做了有益的探索.     

钼-铌合金原料品质对单晶制备的影响

主要讨论了钼-铌合金原料品质,包括烧结条的制备、原料的化学成分、原料棒的尺寸规格等对单晶制备的影响。结果表明:高温真空烧结钼-铌合金烧结条由于C、O等杂质含量过高,在20 kW电子束悬浮区域熔炼炉上区域熔炼时未能直接生长制备出单晶,但其经过两次电子束熔炼获得的Ф(12~17)mm原料棒C元素质量分数降为6.3×10-3%、O元素质量分数降低了近2个数量级,仅为1.4×10-3%,能稳定地生长制备出Ф31 mm×735 mm的大尺寸钼-铌合金单晶,而直径超过Ф18 mm或小于Ф11 mm原料棒在区域熔炼时未能获得钼-铌合金单晶。     

CVD-Si3N4陶瓷及其复合材料氧化行为研究进展

概述了CVD—Si3N4陶瓷及其复合材料在干燥氧气下的氧化行为。Si3N4陶瓷在高温下氧化时，除生成SiO2保护膜外，还生成一薄层比SiO2膜更优异的氧气扩散阻挡层(Si—O—N化合物层)，该层具有优异的抗氧化性能。介绍了两种氧化机制模型，同时分析了温度、杂质等对CVD—Si3N4陶瓷氧化行为的影响。     

基于Solid Works和Cosmos的模具结构三维设计及有限元分析

复杂结构注塑模具的设计和强度、刚度分析是注塑行业的重要难题。利用Solid Works三维设计软件实现了注塑模具的三维实体建模，并运用COSMOS／Works软件对注塑模具的典型部件进行了有限元分析，验证设计的零件是否符合实际工作情况是实现注塑模具现代化设计的重要途径。通过GearTrax2001Plus、Toolbox等外挂、内挂插件的使用．大大地简化了建模过程，克服了原有设计方法的不足．为解决较复杂的结构设计和理论分析问题提供了一种新的途径。     

基于FW-H方程的旋翼气动声学计算研究

由流体力学N S方程导出的非齐次波动方程———FfowcsWilliams Hawkings方程(简称FW H方程),可以精确地描述在静止流体中运动的物体与流体相互作用的发声问题。以FW H方程为理论模型,将旋翼桨叶运动发声问题等效为包含桨叶的任意运动控制面(声源面)的声辐射问题,并在旋翼绕流Euler方程数值模拟的基础上,在时域内计算了悬停旋翼和前飞旋翼的声场。应用于UH 1H和AH 1/OLS两种旋翼模型的气动声学计算表明:计算结果与噪声实验值符合良好;所研制的程序不仅能够较准确地计算单极子噪声和偶极子噪声,而且具有较强的跨音速四极子噪声预测能力。     

Deep Impact: Working Properties for the Target Nucleus – Comet 9P/Tempel 1

In 1998, Comet 9P/Tempel 1 was chosen as the target of the Deep Impact mission (A’Hearn, M. F., Belton, M. J. S., and Delamere, A., Space Sci. Rev., 2005) even though very little was known about its physical properties. Efforts were immediately begun to improve this situation by the Deep Impact Science Team leading to the founding of a worldwide observing campaign (Meech et al., Space Sci. Rev., 2005a). This campaign has already produced a great deal of information on the global properties of the comet’s nucleus (summarized in Table I) that is vital to the planning and the assessment of the chances of success at the impact and encounter. Since the mission was begun the successful encounters of the Deep Space 1 spacecraft at Comet 19P/Borrelly and the Stardust spacecraft at Comet 81P/Wild 2 have occurred yielding new information on the state of the nuclei of these two comets. This information, together with earlier results on the nucleus of comet 1P/Halley from the European Space Agency’s Giotto, the Soviet Vega mission, and various ground-based observational and theoretical studies, is used as a basis for conjectures on the morphological, geological, mechanical, and compositional properties of the surface and subsurface that Deep Impact may find at 9P/Tempel 1. We adopt the following working values (circa December 2004) for the nucleus parameters of prime importance to Deep Impact as follows: mean effective radius = 3.25± 0.2 km, shape – irregular triaxial ellipsoid with a/b = 3.2± 0.4 and overall dimensions of ∼14.4 × 4.4 × 4.4 km, principal axis rotation with period = 41.85± 0.1 hr, pole directions (RA, Dec, J2000) = 46± 10, 73± 10 deg (Pole 1) or 287± 14, 16.5± 10 deg (Pole 2) (the two poles are photometrically, but not geometrically, equivalent), Kron-Cousins (V-R) color = 0.56± 0.02, V-band geometric albedo = 0.04± 0.01, R-band geometric albedo = 0.05± 0.01, R-band H(1,1,0) = 14.441± 0.067, and mass ∼7×10¹³ kg assuming a bulk density of 500 kg m⁻³. As these are working values, {i.e.}, based on preliminary analyses, it is expected that adjustments to their values may be made before encounter as improved estimates become available through further analysis of the large database being made available by the Deep Impact observing campaign. Given the parameters listed above the impact will occur in an environment where the local gravity is estimated at 0.027–0.04 cm s⁻² and the escape velocity between 1.4 and 2 m s⁻¹. For both of the rotation poles found here, the Deep Impact spacecraft on approach to encounter will find the rotation axis close to the plane of the sky (aspect angles 82.2 and 69.7 deg. for pole 1 and 2, respectively). However, until the rotation period estimate is substantially improved, it will remain uncertain whether the impactor will collide with the broadside or the ends of the nucleus.