基于磁场映像的印制电路板故障诊断方法研究

简要分析了印制电路板的电磁场，提出了用电磁感应法测量磁场的电咱故障诊断新方法，并给出了测试系统组成方案。最后通过验证实验证明了该方法是确实可行的。     

满足约束的Gn连续过渡曲面的构造

在Erich Hartmann提出的由两基曲面线性组合构造G^n连续过渡曲面方法的基础上，针对该方法存在很难找到合适的参数变换的问题，提出了一种基于基曲面局部区域重新参数化构造G^n连续过渡曲面的方法。通过对基曲面上切触线附近区域部分曲面重新参数化，再由重新参数化局部基曲面线性组合构造G^n连续过渡曲面。这样将两基曲面间构造过渡曲面的问题转化为在重新参数化局部基曲面间构造过渡曲面。以构造G^1连续的翼身融合面为例，讨论了满足约束要求条件时G^2连续过渡面的构造方法。即先对基曲面上过渡切触线附近的局部区域进行重新参数化，后通过优化求解来确定比例因子和偏移量、平衡因子和调配因子，使过渡曲面满足前后边条线约束，最后利用线性组合来构造G^2连续的过渡面。约束过渡曲面的形状可通过改变重新参数化基曲面的大小来调整．     

镉镍电池在武器回收系统中的应用探讨

文章对镉镍电池在武器回收系统中的应用进行了探讨 ,得到了在武器回收系统中可以用镉镍充电电池取代银锌蓄电池的结论     

翼柱型装药发动机点火升压过程计算

利用实验获得的翼槽内火焰传播规律经验公式,在Ｐ（ｔ）模型的基础上,建立了翼柱型发动机的点火升压计算模型。计算结果与实测数据吻合较好。同时就点火器流量、推进剂燃速、喷管堵盖打开压强等设计参数对发动机点火升压过程的影响进行了分析。     

固体火箭发动机点火药量的计算

通过对点火过程及数学模型的描述，以气体状态方程计算点火药量的公式为基础，提出了一个新的点火药量计算经验公式，并讨论了公式的应用情况和使用范围。     

转子分区循环对称接触应力分析

 通过光弹实验表明了端齿连接转子受力的分区循环对称性。针对这~特性建立了各循环对称分区的循环对称接触有限元应力分析方法,并利用叠加原理将各循环对称分区间过渡区化为几个小规模的循环对称问题。     

密封结构中超弹性接触问题的有限元分析方法

给出了不可压缩超弹性橡胶密封材料轴对称大变形的分析计算方法,利用基于接触面的罚单元算法,采用有限元分析方法对固体发动机密封结构进行了计算,对密封界面上的接触压应力分布规律进行了研究,为橡胶密封件的设计计算提供了一条新途径。     

缘板及叶冠间的接触状况及其对叶片位移和应力的影响

1.计算方法及其实验验证 本文用分析法见文献[1],这里以WS9高压二级涡轮转子叶片(简称WS9叶片)为例来说明方法的特点。该转子轮盘上均匀安装110片叶片,组成具有循环对称接触结构的叶片环,有接触表面的循环对称结构。据此,可将图1所示的一片叶片取作基本段分析,但同时必须在该叶片一般有限元刚度方程中引入缘板及叶冠的循环对称接触表面(叶冠的A1侧面与A2侧面,以及缘板的B1侧面与B2侧面)处的循环对称接触     

加热板上蒸发液滴动态特性的实验

采用高速摄像技术可视化观察5 μl小液滴在铜、铝和不锈钢表面上的蒸发与核化过程,板温50～112℃.实验测量了液滴高度、湿润半径和接触角随时间的动态演化.板温低于100℃时蒸发处于自由界面蒸发模态,过程可分为两阶段,第一阶段液滴高度和接触角连续降低,湿润半径仅比初始值略有降低;第二阶段后退角恒定,湿润半径迅速降低至零.板温高于100℃时处于核态沸腾模态,液滴内部核化及气泡动力学过程强烈依赖壁面过热度.自由界面蒸发模态和核态沸腾模态,壁面平均热流与壁温均呈线性关系,斜率的不同反映两种模态换热机制的差别.     

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.