某型无人直升机遥控系统BIT技术研究与实现

机内测试 (Built- In Test,简称 BIT)是一种能显著改善系统或设备测试性和诊断能力的重要技术手段。文中研究如何在遥控系统中运用 BIT技术来提高其测试性 ,并提出了一种分层测试方案 ,研究成果已应用于某型无人驾驶直升机 ,满足了遥控系统的测试性要求     

介质粘性对椭圆齿轮流量计性能影响的研究

本文根据粘性流体力学原理和转子动力学理论,分析了椭圆齿轮流量计的缝隙漏流和转子受力状况,建立了能预测介质粘性对流量计误差特性和压力损失影响的理论模型。数值计算表明,理论值与实验数据基本吻合。     

直升机红外抑制器两种进气方式下的实验研究

利用地面模拟试验件通过实验比较分析了两种进气方式对红外抑制器性能的影响。为了模拟直升机前飞和悬停两种状态,在模型上端开口,分别引入旋翼下洗气流和前端进气,对比分析了这两种状态下模型壁面温度和红外辐射强度的大小。结果表明:引入速度为18 m/s的旋翼下洗气流使得模型壁面内外两侧均受到冷却气膜的保护,从而使壁面温度降低了36%;同时再引入流量为0.2 kg/s的前端进气,可使红外抑制器模型在3~5μm和8~14μm的红外辐射强度分别降低为原来的11%和28%。     

一种分析轮式起落架直升机“舰面共振”的方法

 针对轮式起落架直升机，提供了一种“舰面共振”动力稳定性分析方法。首先，针对直升机在舰面上随舰船一起摇晃时左右起落架受载不对称的状况，近似采用受对称载荷产生对称变形、受非对称载荷产生非对称变形的方法计算了直升机的平衡状态；其次，根据轮式起落架轮胎和缓冲支柱刚度和阻尼共同作用的特点，结合轮式起落架的几何关系，采用复刚度的方法得出起落架作用于机体的刚度与阻尼；最后，用桨叶振动模态法对轮式起落架的直升机进行了不同旋翼升力卸载以及鱼叉系留与否的“舰面共振”动力稳定性计算分析，并通过算例得到验证。     

三维机身起落架着陆冲击力学模型

 本文根据起落架系统的几何、运动学及动力学特性,推导出目前广泛使用的三维机身式起落架,并具有柔性支柱系统的着陆冲击力学模型。并对其初始条件、对称着陆及不对称着陆情况作了动力学分析。     

不均布行星齿轮传动装置设计的几个问题

推导了不均布行星传动的装配条件；提出了不均布所带来的各行星轮合力及工作过程中的动不平衡离心力的计算公式；推荐了使其合力为零或减至最小的方法；得出了行星轮不均布的行星传动装置的使用条件和设计时应注意的几个问题。     

起落架与防滑刹车系统的相互作用研究

通过采用一个简化的起落架数学模型,对某机在着陆滑跑过程中防滑刹车系统的工作状态进行计算机仿真;并通过改变起落架的结构参数,对起落架与刹车系统在飞机着陆刹车过程中的相互作用进行了初步的定量分析,最后提出了考虑起落架因素的刹车系统半物理仿真试验验证方法。     

直升机复合材料桨叶修理

介绍了某型直升机复合材料桨叶缺陷、损伤的检测方法和复合材料桨叶的修理方法,并叙述了桨叶修理后的试验。     

飞机支柱式起落架落震仿真及缓冲器优化分析

主要介绍支柱式起落架缓冲器的各个参数,包括缓冲支柱的初压力、初容积、油孔面积、活塞面积、缓冲支柱行程等。介绍起落架落震时缓冲器轴向载荷的计算公式。结合具体飞机型号利用初始参数通过AD-AMS软件建立数值模型并进行仿真分析,计算结果与试验结果比较,发现两者具有较好的一致性。最后以起落架缓冲器的油孔面积作为设计参数进行优化分析,给出最优值。     

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.