金属弹簧管性能影响因素的仿真分析

为了研究高温密封组件金属弹簧性能,本文通过对波音公司编网状弹簧管结构和Streck心脏支架结构的研究,建立了编织弹簧的几何拓扑构型和数学模型,推导了弹簧直径计算公式。采用AUTODESK3D-MAX构建了编织弹簧的仿真模型,用ANSYS仿真软件分别从编织丝直径、编织密度以及编织方法 3方面探究不同测试对弹簧性能的影响。结果表明,增加弹簧丝直径、降低弹簧管轴向方向的编织密度、提高圆周方向的编织密度、向外的弹簧管编织方式可有效提高弹簧管的回弹性能。     

基于功能检测的备用系统维修优化研究

为了减小或消除主系统故障的后果,机械中经常采用备用系统在主系统故障时代替其完成功能。根据某些机械设备的备用系统故障具有延迟性的特点,提出了不等间隔的功能检测策略;建立了该策略下备用系统的可用度模型和费用率模型;以系统可用度为约束,维修费用率为目标,建立了不等间隔功能检测维修策略下的维修优化模型;最后给出了优化模型的求解算法,得到了维修间隔的确定方法并进行了实例验证分析,结果表明：当首次检测间隔是重复检测间隔的3倍时采用不等间隔的功能检测优化模型比采用等间隔的功能检测优化模型节约9.55%。     

基于Lamb波相控阵和图像增强方法的损伤监测

利用Lamb波和超声相控阵理论对结构进行损伤监测。选择合适的低频窄带激励信号,产生单一模式Lamb波,结合超声相控阵技术对结构进行多方位监测。针对原始损伤图像不完美的问题,研究基于点运算的对比度增强方法,改善图像质量,提高图像的可识别度和分辨率。在复合材料板结构和铝板结构中针对不同损伤类型的实验研究证明,运用图像增强技术后的损伤图像表征清晰、识别度高。     

二维超燃冲压发动机磁控进气道的数值模拟

针对飞行马赫数大于设计马赫数的情况,采用二维磁流体动力学方程对磁控进气道进行了数值模拟研究。数值模拟结果表明磁流体装置的电磁作用可以使非设计马赫数下进气道激波满足SOL(shock on lip)条件,并使出口处的流动变得均匀。分析了磁流体作用位置、宽度和深度等关键控制参数对该类进气道性能的影响,计算结果表明,磁流体作用区域越靠近飞行器前缘,而且在纵向越深,则进气道出口处的流动越均匀,但流率会有所下降;若磁流体作用区域较宽,则需较小的磁场就能使非设计马赫数下进气道的激波结构满足SOL条件。     

MHD加速器模式磁控进气道的优化设计

为提高超燃冲压发动机进气道在非设计状态下的性能,对磁控进气道进行了研究。采用二维磁流体动力学(MHD)模型对加速器模式的磁控进气道进行了数值模拟和参数优化。分析了电磁作用使空气流率增加的原因,选取了一组优化的设计参数进行数值模拟,确定了磁流体关键参数与进气道主要性能参数的匹配原则。分析表明磁场的大小和方向以及电磁作用的位置对进气道性能有重要影响;唇口附近及上方的电磁作用对增加空气流率起到了关键的作用,磁流体加速器可以显著增加进气道的空气捕获率和压缩比,但由于不可逆效应总压恢复系数会减小。研究结果表明,当飞行马赫数小于设计马赫数时加速器模式的磁控进气道可以提高进气道的性能。     

金属粉末熔化快速成型技术的研究进展

SLM技术代表了快速制造领域的发展方向,运用该技术能直接成型复杂结构、高尺寸精度、高表面质量的致密金属零件,减少制造金属零件的工艺过程,为产品的设计、生产提供更加快捷的途径,进而加快产品的市场响应速度,更新产品的设计理念和生产周期.SLM技术在未来将会得到更好、更快的发展.     

泡沫夹层结构复合材料准静态压痕实验

研究了两种芯材高度的泡沫夹层结构复合材料在准静态压痕力下的损伤过程与形式,通过控制压头位移得到位移与接触力的关系曲线以及不同位移下的损伤形貌,比较了两种芯材的损伤过程.结果表明:损伤过程为泡沫塌陷、泡沫芯材出现裂纹、夹层板上蒙皮分层和芯材与下蒙皮脱粘;损伤形式为:厚芯材时裂纹与泡沫厚度方向成±45.,薄芯材时裂纹与泡沫厚度方向成90°.     

The Magnetic Field of Mercury

The magnetic field strength of Mercury at the planet’s surface is approximately 1% that of Earth’s surface field. This comparatively low field strength presents a number of challenges, both theoretically to understand how it is generated and observationally to distinguish the internal field from that due to the solar wind interaction. Conversely, the small field also means that Mercury offers an important opportunity to advance our understanding both of planetary magnetic field generation and magnetosphere-solar wind interactions. The observations from the Mariner 10 magnetometer in 1974 and 1975, and the MESSENGER Magnetometer and plasma instruments during the probe’s first two flybys of Mercury on 14 January and 6 October 2008, provide the basis for our current knowledge of the internal field. The external field arising from the interaction of the magnetosphere with the solar wind is more prominent near Mercury than for any other magnetized planet in the Solar System, and particular attention is therefore paid to indications in the observations of deficiencies in our understanding of the external field. The second MESSENGER flyby occurred over the opposite hemisphere from the other flybys, and these newest data constrain the tilt of the planetary moment from the planet’s spin axis to be less than 5°. Considered as a dipole field, the moment is in the range 240 to 270 nT-R _M ³ , where R _M is Mercury’s radius. Multipole solutions for the planetary field yield a smaller dipole term, 180 to 220 nT-R _M ³ , and higher-order terms that together yield an equatorial surface field from 250 to 290 nT. From the spatial distribution of the fit residuals, the equatorial data are seen to reflect a weaker northward field and a strongly radial field, neither of which can be explained by a centered-dipole matched to the field measured near the pole by Mariner 10. This disparity is a major factor controlling the higher-order terms in the multipole solutions. The residuals are not largest close to the planet, and when considered in magnetospheric coordinates the residuals indicate the presence of a cross-tail current extending to within 0.5R _M altitude on the nightside. A near-tail current with a density of 0.1 μA/m² could account for the low field intensities recorded near the equator. In addition, the MESSENGER flybys include the first plasma observations from Mercury and demonstrate that solar wind plasma is present at low altitudes, below 500 km. Although we can be confident in the dipole-only moment estimates, the data in hand remain subject to ambiguities for distinguishing internal from external contributions. The anticipated observations from orbit at Mercury, first from MESSENGER beginning in March 2011 and later from the dual-spacecraft BepiColombo mission, will be essential to elucidate the higher-order structure in the magnetic field of Mercury that will reveal the telltale signatures of the physics responsible for its generation.