超机动性技术及其战术优势探讨

随着对新型战机机动性要求的提高及飞机在大迎角下过失速状态的深入研究,提出了新型战机的超机动性技术。首先对超机动性的技术内涵、判断准则做简要介绍,然后对现代近距空战中,战机采用超机动性技术可能取得的战术优势及可能存在的一些问题进行了分析探讨。     

军机研制信息资源共享问题初探

对国内外军机研制信息资源共享与应用情况进行了分析 ,研究了国外广泛采用的CALS战略体系 ,并就结合CALS理论用于解决我国军机研制信息资源共享存在的问题进行了初步探讨 ,提出了相关建议     

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     

再入式光纤陀螺实用化技术研究

再入式光纤陀螺（Re—FOG）使相互干涉的两路光循环进入光纤环，通过缩短光纤长度克服温度和应力引起的误差。本文研究了再入武光纤陀螺实用化的相关技术；提出了一种采用脉冲相位调制的信号检测方法；设计了专门的数据通讯模块。实验结果表明：所提出的信号检测方法可分离出所需循环次数的信号并解算出陀螺转速；所设计的通讯模块能保证实现陀螺与导航计算机之间的快速、稳定、准确的数据传送。再入式光纤陀螺可成为实用化的新型光纤陀螺。     

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。     

某型战机滑跃起飞性能初步分析

根据飞行动力学理论,建立了舰载机滑跃起飞数学模型。以某型战机为例进行了数值仿真,定量分析了起飞质量、起飞迎角、甲板风、滑跑距离等因素对滑跃起飞性能的影响。结果表明:应优选起飞迎角;不同起飞质量情况下,应选择合适的滑跑距离(起飞点),并保证适当的甲板风;起落架强度应加强。     

短纤维增强复合材料纤维和界面层残余热应力分析

基于应力传递的剪滞理论，详细分析推导了纤维中的残余热正应力和界面层中的剪应力解析公式，并与已有的理论公式进行了比较。同时分析了纤维与基体脱粘的原因及热残余应力主要影响因素，主要包括：纤维和界面层材料的弹性模量，界面层的厚度以及纤维的长径比等。通过分析得出：纤维中的压应力和界面层中的剪应力都随着界面层的厚度及其弹性模量的增大而增大；纤维长径比的大小对纤维中的压应力和界面层中的剪应力大小及分布的影响很小。     

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.