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。     

三维喷管设计

为了简化设计过程并获得满意的设计性能，以圆转方和圆转矩形喷管为例，对已有的三维喷管型面设计方法进行比较和总结，运用数值方法分析了型面转换起始位置和喷管出口高宽比的确定，提出了一套三维型面的直接生成方法，并给出相应的设计准则。经过实际设计和加工的检验，证明了设计方法的工艺可行性。在能够保证三维喷管的制造工艺条件以及冷却通道布置要求下，型面转换的起始位置可以尽量接近喉部；喷管出口截面的宽边不要超过窄边的1．5倍，应尽量接近于方形。     

计算机在固体火箭发动机设计与研制中的应用

随着计算机在分析与仿真中的广泛应用,固体火箭发动机工作过程中许多复杂而难以观察的现象已能得到揭示.因此,计算机的应用已成为设计与研制高性能固体火箭发动机的十分重要的手段.本文综述了应用计算机在一些固体火箭发动机的性能预示、设计优化、性能检验和故障分析等方面所取得的成就,并就今后我国在设计与研制固体火箭发动机中如何加强计算机化提出了若干建议.     

近代大型液体火箭发动机的特点

本文对近代大型液体火箭发动机的特点进行了综述和分析.文中指出:使用高能、无毒的液氧、煤油和液氧、液氢为大型液体火箭发动机的推进剂势在必行;采用高压补燃循环系统可以明显提高发动机的比冲、减小发动机尺寸和质量;采用推进剂利用系统可以减少推进剂的剩余量,以提高运载火箭的有效载荷;使用辅助增压泵可降低贮箱压力,并提高发动机主泵的入口压力,以保证主泵在没有汽蚀的条件下可靠工作;高可靠性、长寿命和重复使用对航天产品尤为重要.     

两级固体火箭联合动力装置的参数优化

本文针对某型导弹由两级固体火箭发动机组成的联合动力装置进行九变量寻优计算.通过采用二维抛物线插值方法及合理组织迭代的技巧,解决了庞大的目标函数计算子程序耗时太多的问题;经大量调试,协调寻优步长、罚因子、收敛精度,最后成功地完成了本文的九维寻优计算,得到了能稳定收敛的最优解.所得最优方案比原参考方案的发动机总重减轻7.03kg(约占总重的2%).     

旋转同心双轴间流动的热态实验

某型发动机高、低压涡轮轴间环形气流通内的流动可以简化为两个独立旋转同心双轴环道内的流动问题。对其控制方程以及边界条件进行无量纲化，得出了实验准则，设计并建立了实验台，以实验方法研究了具有轴向通流的独立旋转同心双轴环道内的流动规律。结果表明，随着冷气雷诺数增大，阻力系数总体趋势减小；冷气雷诺数的影响远大于内轴和外轴旋转对流动的影响。     

涡轮发动机聚氧减重探索

本文在聚氧提高航机部件性能，总体性能的研究基础上，进一步探索航空发动机聚氧减重的规律，提供聚氧缩短压气机、燃烧室、涡轮轴向尺寸、减少发动机直径、减轻上述核心机部件和发动机总重量的理论依据，可供航机预研参考。     

基于解析及特征造型的涡轮冷却叶片参数化设计

基于数学解析与特征造型技术相结合的方法,建立了基于构造过程的复杂涡轮冷却叶片的参数化设计技术。用五次多项式描述叶身型线,根据壁面厚度函数求解冷却通道外形,定义冷却通道隔板位置及厚度等参数,计算得到叶身及冷却通道各截面造型数据;以特征造型方法完成对涡轮冷却叶片转弯流道、缘板、榫头及叶片相关特征的参数化设计;利用CAD系统的二次开发接口,实现了多腔回流式涡轮冷却叶片的自动建模。     

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.