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Solid Works和Cosmos的模具结构三维设计及有限元分析

复杂结构注塑模具的设计和强度、刚度分析是注塑行业的重要难题。利用Solid Works三维设计软件实现了注塑模具的三维实体建模，并运用COSMOS／Works软件对注塑模具的典型部件进行了有限元分析，验证设计的零件是否符合实际工作情况是实现注塑模具现代化设计的重要途径。通过GearTrax2001Plus、Toolbox等外挂、内挂插件的使用．大大地简化了建模过程，克服了原有设计方法的不足．为解决较复杂的结构设计和理论分析问题提供了一种新的途径。     

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.     

农林飞机结构抗坠毁设计技术

农林飞机通常在3-5m的超低空进行作业飞行,在离地面3m以上的空中往往会有树木、电线杆、电线、堤坝、土堆、山丘、建筑物等障碍物,稍有不慎,就有与之撞击的可能。这样的工作条件除要求飞机具有良好的超低空飞行性能以外,还要求飞机具有一定的耐坠撞能力。本文针对农林飞机执行任务过程中可能发生的碰撞、坠毁等特点,研究了农林飞机抗坠毁设计技术、计算分析仿真技术。     

可重复使用运载器磁悬浮助推发射参数研究

针对磁悬浮助推水平起飞运载器这种新型发射概念,采用概念性分析方法,研究地面发射参数对可重复使用运载器性能的影响规律。结果表明,助推发射水平起飞运载器在降低初始推重比、推进剂和结构质量等方面具有优势,最后得出地面发射参数的一组优化值。     

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.     

一个通用的微型飞行器气动工程估算环境的开发

针对微型飞行器 (MicroAirVe hicle,简称MAV)多学科设计优化的需要 ,本文以MAV工程估算的三层模型描述为基础 ,开发了一个通用的MAV气动工程估算程序 ,它可以对多种布局MAV进行气动参数的计算 ,并且MAV几何外形的描述简单 ,计算方便正确 ,最后对某MAV的气动估算结果与风洞实验曲线进行了比较。     

复合材料旋翼桨叶研制中的几个问题分析

本文针对复合材料旋翼桨叶的主要特点,结合国内自行设计研制的复合材料桨叶设计及制造过程中遇到的几个实际问题及处理措施进行了较详细的介绍,并对复合材料桨叶开发研制提出了一些建议。     

智能化多传感器管理系统的设计和仿真

根据机载多传感器管理需求,提出了基于机载多传感器数据融合技术的智能化多传感器管理系统体系结构,并阐述了该系统的功能、系统设计原则和方法。采用商用货价产品技术(COTS)构建原型仿真平台,对提出的多传感器管理系统体系结构进行原型仿真,验证了该设计的有效性。     

基于欧拉方程的跨声速翼型设计

给出了一种基于欧拉方程的跨声速翼型设计方法。方法以Ｔａｋａｎａｓｈｉ提出的“正反迭代余量修正”设计原理为基础，在气动力分析模块中，以欧拉方程为基本控制方程，并采用Ｗａｌｚ边界层方法对其进行粘性修正；反设计模块采用经过改进的二维翼型设计方法。方法的程序经过几个设计实例主题证明是有效而实用的。