滑流区中三角翼大攻角气动力特性的实验研究

一种以后掠75.7°薄三角翼为主要特征的典型航空航天飞行器模型,在激波管风洞马赫数为11.9和15.4两种条件下,攻角范围20°～50°,用模型自由飞方法测量了它们的轴向力系数、法向力系数和俯仰力矩特性。相应的实验雷诺数分别为3.19×10~4和1.64×10~4,这两种流动条件均属于稀薄气流的滑流区。 实验结果表明在M_∞=11.9和15.4两种条件下,两种剖面外形模型的升力系数和阻力系数均随攻角加大而递增,其变化规律有很好的一致性,且对马赫数并不敏感;但从体轴系来看,不仅两种模型的轴向力系数不同,而且因粘性干扰的缘故,同一模型A在M_∞=15.4时比M_∞=11.9时有相对较大的轴向力系数,但两者随攻角变化的规律一致,且当α>45°时接近牛顿值。此外,实验表明两种模型的压心系数随攻角均没有明显变化。     

Magnetosphere Imaging Instrument (MIMI) on the Cassini Mission to Saturn/Titan

The magnetospheric imaging instrument (MIMI) is a neutral and charged particle detection system on the Cassini orbiter spacecraft designed to perform both global imaging and in-situ measurements to study the overall configuration and dynamics of Saturn’s magnetosphere and its interactions with the solar wind, Saturn’s atmosphere, Titan, and the icy satellites. The processes responsible for Saturn’s aurora will be investigated; a search will be performed for substorms at Saturn; and the origins of magnetospheric hot plasmas will be determined. Further, the Jovian magnetosphere and Io torus will be imaged during Jupiter flyby. The investigative approach is twofold. (1) Perform remote sensing of the magnetospheric energetic (E > 7 keV) ion plasmas by detecting and imaging charge-exchange neutrals, created when magnetospheric ions capture electrons from ambient neutral gas. Such escaping neutrals were detected by the Voyager l spacecraft outside Saturn’s magnetosphere and can be used like photons to form images of the emitting regions, as has been demonstrated at Earth. (2) Determine through in-situ measurements the 3-D particle distribution functions including ion composition and charge states (E > 3 keV/e). The combination of in-situ measurements with global images, together with analysis and interpretation techniques that include direct “forward modeling’’ and deconvolution by tomography, is expected to yield a global assessment of magnetospheric structure and dynamics, including (a) magnetospheric ring currents and hot plasma populations, (b) magnetic field distortions, (c) electric field configuration, (d) particle injection boundaries associated with magnetic storms and substorms, and (e) the connection of the magnetosphere to ionospheric altitudes. Titan and its torus will stand out in energetic neutral images throughout the Cassini orbit, and thus serve as a continuous remote probe of ion flux variations near 20R _S (e.g., magnetopause crossings and substorm plasma injections). The Titan exosphere and its cometary interaction with magnetospheric plasmas will be imaged in detail on each flyby. The three principal sensors of MIMI consists of an ion and neutral camera (INCA), a charge–energy–mass-spectrometer (CHEMS) essentially identical to our instrument flown on the ISTP/Geotail spacecraft, and the low energy magnetospheric measurements system (LEMMS), an advanced design of one of our sensors flown on the Galileo spacecraft. The INCA head is a large geometry factor (G ∼ 2.4 cm² sr) foil time-of-flight (TOF) camera that separately registers the incident direction of either energetic neutral atoms (ENA) or ion species (≥5^∘ full width half maximum) over the range 7 keV/nuc < E < 3 MeV/nuc. CHEMS uses electrostatic deflection, TOF, and energy measurement to determine ion energy, charge state, mass, and 3-D anisotropy in the range 3 ≤ E ≤ 220 keV/e with good (∼0.05 cm² sr) sensitivity. LEMMS is a two-ended telescope that measures ions in the range 0.03 ≤ E ≤ 18 MeV and electrons 0.015 ≤ E≤ 0.884 MeV in the forward direction (G ∼ 0.02 cm² sr), while high energy electrons (0.1–5 MeV) and ions (1.6–160 MeV) are measured from the back direction (G ∼ 0.4 cm² sr). The latter are relevant to inner magnetosphere studies of diffusion processes and satellite microsignatures as well as cosmic ray albedo neutron decay (CRAND). Our analyses of Voyager energetic neutral particle and Lyman-α measurements show that INCA will provide statistically significant global magnetospheric images from a distance of ∼60 R _S every 2–3 h (every ∼10 min from ∼20 R _S). Moreover, during Titan flybys, INCA will provide images of the interaction of the Titan exosphere with the Saturn magnetosphere every 1.5 min. Time resolution for charged particle measurements can be < 0.1 s, which is more than adequate for microsignature studies. Data obtained during Venus-2 flyby and Earth swingby in June and August 1999, respectively, and Jupiter flyby in December 2000 to January 2001 show that the instrument is performing well, has made important and heretofore unobtainable measurements in interplanetary space at Jupiter, and will likely obtain high-quality data throughout each orbit of the Cassini mission at Saturn. Sample data from each of the three sensors during the August 18 Earth swingby are shown, including the first ENA image of part of the ring current obtained by an instrument specifically designed for this purpose. Similarily, measurements in cis-Jovian space include the first detailed charge state determination of Iogenic ions and several ENA images of that planet’s magnetosphere.This revised version was published online in July 2005 with a corrected cover date.     

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。     

旋翼塔信号传输系统干扰的排除方法

旋翼塔信号传输系统是旋翼塔测试系统的重要组成部分,信号传输质量是决定测试系统测试数据真实性的最重要因素。由于旋翼试验塔采用长线传输,所以必须排除信号传输系统的干扰,必须对信号传输系统进行调试,以确保试验数据的可靠和准确。     

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.     

直升机尾桨故障及其试飞研究

介绍了直升机尾桨故障类型及其处理方法和试飞方法。探讨了发动机功率、空速、飞行高度等因素对尾故障试飞的影响。在实际试飞的基础上，给出了正确处理尾桨故障的基本方法，为直升机飞行员在飞行时遇到类似故障后的处理及有关研究人员提供了重要的参考。     

芳纶纤维／环氧复合材料界面超声连续改性处理

运用超声技术在芳纶/环氧复合材料制备过程中对其界面进行改性处理,分析了超声处理过程中纤维与树脂之间浸润性的变化趋势以及超声作用对复合材料界面性能和力学性能的影响。结果表明:超声是通过改善纤维与树脂之间的浸润性,提高复合材料的界面性能及力学性能。     

基于BP人工神经网络的GPS／SINS组合导航算法

基于扩展Kalman滤波的GPS／SINS组合导航算法，需要对原始的非线性连续系统模型进行线性化和离散化处理，要求系统噪声和测量噪声为零均值的高斯白噪声，且易于出现滤波器发散。BP人工神经网络毋需对所求解的问题建模，能够很好地逼近系统非线性特性，获得较高精度的导航定位信息；还具有计算过程稳定，不涉及矩阵求逆，不需要迭代逼近，以及容易实现并行处理等优点。本文设计适用于GPS／SINS组合导航系统的BP网络模型，并在标准的BP算法基础上，采用共轭梯度法改进网络训练速度及精度。最后，通过仿真算例说明BP网络方法用于GPS／SINS组合导航计算的可行性。     

全面国产化复合材料在XX旋翼国产化中的应用研究

本文概要地介绍了国产复合材料在XX旋翼国产化的应用研究总体思路,分析了国产复合材料的研究现状。通过国产化复合材料在旋翼桨叶上的设计应用分析,确定了国产材料性能的最低要求,并进行了典型样件—模型桨叶的验证考核。     

粘流与无粘流的相互作用计算

本文总结了粘流/无粘流的各种计算方法和结果。重点在于介绍定常流动中的弱相互作用。首先叙述了弱相互作用的数学模型。给出了不可压流动和跨音速流动中粘流/无粘流相互作用的某些正耦合的计算结果。讨论了在分离区附近边界层正方法失效的原因。然后介绍了边界层反方法和适用于带分离的流动中半反方法耦合的粘流/无粘流的相互作用方法。文中也简单地总结了三维情况的应用和强相互作用。