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。     

资源节约型国民经济体系的构建

资源节约型的国民经济体系是资源节约型社会的基础。构建资源节约型国民经济体系，应重点做好以下几个方面的工作：提高全民族的资源忧患意识和节约意识，树立资源节约型观念；把节约资源作为优化结构的重要目标，逐步建立节约型的产业结构和消费结构；构建自律高效的管理体制，着力建设资源节约型主体；完善价格机制、投入机制和补偿机制，建立资源节约型体制和机制；大力发展循环经济和清洁生产，实现资源节约型的经济增长方式；树立科学合理的消费观念，倡导节约型消费方式；建设资源节约型经济调控与监督体系。     

国内外危险品航空运输管理体系的探讨

以荷兰、德国为例,对其危险物品航空运输的法律体系、培训、管理机构与监察制度等方面进行了分析.这两个国家代表了欧洲危险物品航空运输的体制不同却同样有效的管理模式.通过与中国现状比较分析,得出中国民航危险品航空运输在上述方面已接近,甚至在某些方面超过发达国家水平,中国民航有能力确保危险品航空运输安全.     

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。     

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。     

含能工质激光烧蚀推进效率分析

为了分析在高能脉冲激光作用下,含能工质化学能对推进性能的影响,在实验的基础上,对固体含能工质激光烧蚀推进过程中的能量效率进行了初步分析。结果表明:含能工质自身化学能在激光推进中具有重要的作用;与火箭推进方式相比,固体含能材料激光烧蚀推进方式的能量利用效率更高。     

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.