整体壁板损伤容限特性与修理技术研究

用有限元和断裂力学方法分析大型飞机机身整体壁板的破损安全特性。以一个十四桁条的铝合金整体加筋板为例,计算了裂纹从中部蒙皮向两侧均匀扩展并跨过筋条的应力强度因子,并和相同构型的铆接壁板进行了结构对比。应用ANSYS对整体壁板及损伤后双面修补壁板进行有限元分析。研究不同厚度补片对损伤壁板、修补长桁、内外补片受力的影响。选取典型位置研究局部刚度加大对整体壁板传力特性的影响。     

复合材料构件成型模具的参数化设计

文摘实现复合材料构件成型工装的快速设计对缩短生产准备时间、提高构件质量具有重要意义。本文分析了复合材料构件成型模具的结构和建模特点及要求,提取了结构各部分的设计参数;基于CATIA和CAA平台开发了复合材料构件成型模具设计系统,并应用于飞机复合材料构件的成型模具设计中,验证了本文方法的可行性。     

浅析复合材料框架式成型模具设计技术

对于大尺寸复合材料零件成型所用的大型框架式模具,在设计过程中需要使模型建模及更改快速化,需要详细分析模具在实际使用工况下的应力及变形、模具在固化过程中的温度分布及变形情况,并在设计过程中考虑尺寸补偿及回弹补偿,以使模具设计达到高效、精准、优化的目的;使模具结构更好地满足复材零件成型精度要求.     

加筋壁板VARI整体成型工艺设计与验证术

针对一种典型复合材料加筋壁板,完成模具结构及工艺流程等整体成型工艺设计,同时利用PAM-RTM软件完成流道设计优化模拟,并根据模拟结果选择合理的注射方式及流道布局,最终根据所选方案完成工艺试验验证,对构件进行超声无损检测,检测结果显示构件没有内部缺陷、树脂充分填充,最终验证了加筋壁板整体成型工艺设计及模拟分析的有效性.     

加筋壁板VARI整体成型工艺设计与验证

针对一种典型复合材料加筋壁板,完成模具结构及工艺流程等整体成型工艺设计,同时利用PAM-RTM软件完成流道设计优化模拟,并根据模拟结果选择合理的注射方式及流道布局,最终根据所选方案完成工艺试验验证,对构件进行超声无损检测,检测结果显示构件没有内部缺陷、树脂充分填充,最终验证了加筋壁板整体成型工艺设计及模拟分析的有效性。     

水平安定面外伸段壁板结构设计

随着民用航空事业的发展和民用飞机巨大的市场需求,整体壁板结构开始应用在民用支线飞机上。首先介绍支线飞机水平安定面外伸段壁板结构设计的方法。然后根据某支线飞机水平安定面的总体、适航、重量、强度、刚度等要求,进行水平安定面外伸段壁板结构的初步设计,选定水平安定面上下壁板的结构布置方案,根据公式及工程经验,确定壁板的基本几何尺寸,经过强度校核和几轮迭代,得到满意的基本尺寸。进入详细设计阶段,考虑壁板的疲劳、损伤容限、工艺性、防腐性等细节问题,通过强度校核,最终设计出满足多方面要求并且重量较轻的水平安定面外伸段壁板。水平安定面外伸段壁板结构设计对相似机型的结构设计具有参考作用。     

基于UG曲轴锻造模具设计

通过分析复杂多拐曲轴零件的锻造工艺特点,确定了成型工艺方案;运用UG对曲轴进行三维建模,完成了滚挤、弯曲、预锻和终锻模具的设计;实现了曲轴模具的数字化设计,达到模具设计要求、试模一次成功。     

一种新型泡沫填充T型加筋壁板液体成型共固化工艺研究

选取典型复合材料T型加筋壁板结构件,针对其真空辅助液体成型工艺共固化T型加筋壁板铺贴过程中加筋区填充困难、工艺复杂、不可重复等问题,提出了一种针对阴模成型的新型泡沫填充T型加筋壁板共固化成型工艺方法,采用泡沫加筋芯与纤维铺覆导向板,实现了加筋区尺寸精确控制,解决了阴模加筋区填充困难,表面成型质量差的问题,并在注胶过程中引入钢制均压板,采用单面模具得到双面光滑的T型加筋壁板结构件,研制出的加筋壁板成型质量良好,研究结果对壁板类结构低成本整体成型技术在民机上的应用与发展具有重要参考价值。     

复合材料热压罐固化框架式成型模具的参数化设计

为解决复合材料热压罐固化框架式成型模具设计过程中重复性工作较多、设计效率较低、后续修改困难等问题,将参数化设计技术分为尺寸和拓扑结构的参数化设计两个方面,并运用于模具设计中。模具尺寸的参数化设计在分析模具结构特点的基础上,提取出模具的主要设计参数,利用自顶向下的设计思路规划了模具的参数化设计流程;引入参数追溯概念,提出对主要设计参数进行追溯的方法,以便通过参数驱动模具尺寸的快速修改。模具拓扑结构的参数化设计结合CATIA的知识工程模块与面向对象的技术,实现参数化变更模具的拓扑结构。基于CATIA CAA二次开发平台,开发了复合材料固化框架式成型模具参数化设计系统,并给出实例验证。     

飞机复合材料构件成型模具型板架参数化设计

针对复合材料构件成型模具的结构,分析其型板架的设计要求与建模特点,运用参数化设计方法,对结构各部分尺寸建立参数关联,设计了型板的智能排布和散热孔的对齐算法,基于CATIA二次开发平台,开发了复合材料构件成型模具型板架参数化设计模块,应用于飞机复合材料构件的成型模具设计中,可减少模具设计重复性工作,提高设计效率。     

捷变频磁控管用高频直线振荡电机设计

捷变频磁控管的快速捷变特性取决于驱动电机的性能,要求电机功耗小、体积小、效率高,能实现高频稳幅直线振动.文章介绍了音圈直线电机、电磁开关式直线电机和电磁混合式直线电机等三种方案,通过对其工作原理和性能特点分析,确定了音圈直线电机驱动方案,进行了电磁场仿真分析和电磁参数设计,进行了样机试验测试.结果表明,设计的音圈直线电...     

桨叶实度及轴间距对摆线桨气动特性影响研究

悬停状态下,设计参数和摆线桨间距离对摆线桨的气动特性有较大影响。首先通过算例验证滑移网格计算方法应用于摆线桨悬停状态下气动力计算的准确性,然后研究摆线桨在不同半径、弦长和桨叶数时的气动参数特性,最后计算分析不同距离时,摆线桨间的气动干扰特性。结果表明:随着半径增大,桨叶气动力和单位面积上载荷均增大;弦长越大,气动力越大,桨叶单位面积上载荷反而越小;4叶片摆线桨产生的气动力比3叶片和6叶片大,而3叶片的桨叶载荷最大;合力偏转角分别随转速和实度的增大而减小;随着摆线桨间距离的增加,气动力损失系数和合力偏转角均减小。     

A new target tracking filter based on deep learning

At present, current filters can basically solve the filtering problem in target tracking, but there are still many problems such as too many filtering variants, too many filtering forms, loosely coupled with the target motion model, and so on. To solve the above problems, we carry out crossapplication research of artificial intelligence theory and methods in the field of tracking filters. We firstly analyze the computation graphs of typical a-β and Kalman. Through analysis, it is concluded that ...     

Investigations of entrainment characteristics and shear-layer vortices evolution in an axisymmetric rear variable area bypass injector

In this study,firstly,for the axisymmetric RVABI,the change-rule of adverse pressure gradient caused by radial velocity during the transition of internal flow mode in variable geometry is summarized,and a Bypass Ratio(BR) iterative algorithm based on the empirical correlation of non-equilibrium pressure is proposed.The algorithm can estimate the nonlinear relationship between area ratio and BR,with an error range falling below 6.5%.Then,we discuss the favorable effect of uniform mixing on the th...     

PVC糊树脂对交联PVC泡沫塑料的影响

通过水煮发泡制备交联聚氯乙烯泡沫塑料,讨论了聚氯乙烯(PVC)糊树脂对泡沫制备过程中经制糊、模压和发泡工艺得到的产物的影响,研究了PVC糊树脂对制备的交联PVC泡沫压缩性能的影响.结果表明:制备交联聚氯乙烯泡沫塑料适宜的糊黏度是4～9 Pa·s;PVC糊树脂的K值较大或水萃取液pH值呈碱性可有效防止模压过程中PVC的降解;PVC糊树脂的水萃取液pH值呈碱性可催化发泡反应,有利于得到低密度泡沫且缩短发泡时间;随着其K值增加,制备的泡沫压缩强度增大,但是K值过大时,制备的泡沫泡孔较大,压缩强度反而降低,适宜的K值为70～80.     

Alfvénic Electron Acceleration in Aurora Occurs in Global Alfvén Resonosphere Region

Auroral emission caused by electron precipitation (Hardy et al., 1987, J. Geophys. Res. 92, 12275–12294) is powered by magnetospheric driving processes. It is not yet fully understood how the energy transfer mechanisms are responsible for the electron precipitation. It has been proposed (Hasegawa, 1976, J. Geophys. Res. 81, 5083–5090) that Alfvén waves coming from the magnetosphere play some role in powering the aurora (Wygant et al., 2000, J. Geophys. Res. 105, 18675–18692, Keiling et al., 2003, Science 299, 383–386). Alfvén-wave-induced electron acceleration is shown to be confined in a rather narrow radial distance range of 4–5 R _E (Earth radii) and its importance, relative to other electron acceleration mechanisms, depends strongly on the magnetic disturbance level so that it represents 10% of all electron precipitation power during quiet conditions and increased to 40% during disturbed conditions. Our observations suggest that an electron Landau resonance mechanism operating in the “Alfvén resonosphere” is responsible for the energy transfer.     

Multiframe weak target track-before-detect based on pseudo-spectrum in mixed coordinates

Traditional multiframe Track-Before-Detect(TBD) may incur adverse integration loss resulting from model mismatch in sensor coordinates. Its suboptimal integration strategy may cause target envelope degradation. To address these issues, a pseudo-spectrum-based multiframe TBD in mixed coordinates is proposed firstly. The data search for energy integration is conducted based on an accurate model in the x-y plane while target energy is integrated based on pseudo-spectrum in sensor coordinates. The a...     

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.     

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.