基于光滑粒子流体动力学方法的液滴蒸发问题数值模拟研究

基于光滑粒子流体动力学方法（Smoothed Particle Hydrodynamics，SPH），开展了SPH新算法在蒸发燃烧领域的研究。建立了适用于SPH方法的蒸发数值模型，推导了基于傅立叶热传导公式和菲克扩散定律的SPH离散方程；借鉴VOF方法（Volume of Fluid）的思想，提出了SPH粒子的液相质量分数的概念，以有效表征蒸发过程中的相变问题。采用SPH方法对高温环境中单个液滴的蒸发过程进行数值模拟，结果符合D2定律，与理论模型相一致；在强迫对流环境中，液滴的蒸发过程受到对流作用及表面张力的影响，蒸发速率加快；进一步对双液滴在静止、对流环境中的蒸发过程进行数值模拟研究。结果表明，液滴的间距、滴径对多个液滴的蒸发过程影响至关重要，液滴间距至少在两倍的液滴直径以上，相互之间的影响才可以近似忽略。通过本文研究，拓宽了SPH方法在蒸发相变领域的应用范围，研究结果也能够为进一步的燃烧问题研究奠定基础。     

SACMA和QMW试验方法对复合材料层合板低速冲击后压缩行为的影响

采用了 SACMA标准和一种小试样试验方法对复合材料层合板低速冲击后的压缩 (CAI)行为进行试验研究 ,从层合板的冲击损伤分布、冲击后压缩破坏过程 ,以及层合板的准静态横向压缩、开孔后压缩等多方面进行对比 ,结果表明 ,这两种试验方法存在很大差别 ,试验方法不同 ,层合板低速冲击后的压缩行为也不同 ;采用 SACMA标准所测得的低速冲击后压缩强度更能全面反映基体韧性的优劣。作为 CAI试验标准 ,小试样试验方法还有待改进     

氢气泡网格图像测速法—瞬态二维速度场测量

本文介绍一种二维瞬态多点流场测量方法－网格图像测速法。运用数字图像处理技术由氢气泡时间－染色线流动显示图像自动生成网格图像，网格图像的网格结点为氢气泡块角点的拟合点，由网格结点的位移确定流场速度。     

关于刚体转动的角速度和角加速度的讨论

在理论力学教学中，平面运动刚体的转动与基点无关的证明过于简单，本利用矢量代数的知识，证明平面运动刚体的角度与角加速度与基点的选择无关。     

孔子教育哲学中的审美教育方法及现代意义

审美教育是以审美活动为中介，积极塑造人格的特定教育活动，方法上不同于德育与智育。注重审美教育中的情感性和形象性，强调审美情感和理智感、道德感相统一的教育方法，不仅符合审美教育的规律，而且是孔子教育哲学中审美教育实践的一大特色。探析这一特色无疑会对我们今天的教学改革乃至教育目的、过程和实质的研究具有一定的借鉴意义。     

基于视频图像处理的头部位置跟踪方法的探索

针对目前头盔显示器头部位置跟踪过程中存在瞄准速度不快,灵敏度不高,头盔重量偏大,只考虑头部位置,未考虑人眼在跟踪瞄准过程中的功能等问题,特提出一种基于人眼及头位综合视频检测高精度快速瞄准新方法,它采用基于视频图像处理方法来检测头部与飞机的夹角和注视方向相对头部的偏角。     

MESSENGER: Exploring Mercury’s Magnetosphere

The MErcury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) mission to Mercury offers our first opportunity to explore this planet’s miniature magnetosphere since the brief flybys of Mariner 10. Mercury’s magnetosphere is unique in many respects. The magnetosphere of Mercury is among the smallest in the solar system; its magnetic field typically stands off the solar wind only ∼1000 to 2000 km above the surface. For this reason there are no closed drift paths for energetic particles and, hence, no radiation belts. Magnetic reconnection at the dayside magnetopause may erode the subsolar magnetosphere, allowing solar wind ions to impact directly the regolith. Inductive currents in Mercury’s interior may act to modify the solar wind interaction by resisting changes due to solar wind pressure variations. Indeed, observations of these induction effects may be an important source of information on the state of Mercury’s interior. In addition, Mercury’s magnetosphere is the only one with its defining magnetic flux tubes rooted beneath the solid surface as opposed to an atmosphere with a conductive ionospheric layer. This lack of an ionosphere is probably the underlying reason for the brevity of the very intense, but short-lived, ∼1–2 min, substorm-like energetic particle events observed by Mariner 10 during its first traversal of Mercury’s magnetic tail. Because of Mercury’s proximity to the sun, 0.3–0.5 AU, this magnetosphere experiences the most extreme driving forces in the solar system. All of these factors are expected to produce complicated interactions involving the exchange and recycling of neutrals and ions among the solar wind, magnetosphere, and regolith. The electrodynamics of Mercury’s magnetosphere are expected to be equally complex, with strong forcing by the solar wind, magnetic reconnection, and pick-up of planetary ions all playing roles in the generation of field-aligned electric currents. However, these field-aligned currents do not close in an ionosphere, but in some other manner. In addition to the insights into magnetospheric physics offered by study of the solar wind–Mercury system, quantitative specification of the “external” magnetic field generated by magnetospheric currents is necessary for accurate determination of the strength and multi-polar decomposition of Mercury’s intrinsic magnetic field. MESSENGER’s highly capable instrumentation and broad orbital coverage will greatly advance our understanding of both the origin of Mercury’s magnetic field and the acceleration of charged particles in small magnetospheres. In this article, we review what is known about Mercury’s magnetosphere and describe the MESSENGER science team’s strategy for obtaining answers to the outstanding science questions surrounding the interaction of the solar wind with Mercury and its small, but dynamic, magnetosphere.     

弹射救生过程数值计算及损伤风险评估

针对从弹射程序启动到飞行员着陆之间的各个阶段,建立了能够对横滚、俯冲等复杂弹射条件进行计算的数学模型。结合某型座椅的具体参数与气动力数据,针对具体算例求解了弹射救生过程,与实验结果进行了对比。根据模型的计算结果,以动态响应指数(DRI)对不同弹射初速下的损伤风险做出评估,并指出了在不同速度下气动过载的影响。     

金属图象分割的研究

结合金属图象的特点,利用传统阚值分割技术和基于最大熵原则的图象分割技术对金属图象分割进行了分析;并根据金属图象分析要求,提出了先二值化金属图象再进行边缘提取的方法.对比实验结果表明,基于最大熵原则的图象分割技术可以获得较好的分割效果,所提出的方法能够获得连续闭合的晶粒边缘,为下一步的金属图象分析提供了可靠的依据.     

复合材料层板低速冲击剩余强度的研究

 针对复合材料层板受低速冲击后的剩余压缩强度问题进行分析计算,把冲击破坏区看作一个含有随机分布裂纹的圆形不均匀体,采用有限元建模分析,结合冲击后层板的试验所得的载荷/ 位移关系,计算得到冲击破坏区的剩余模量。再采用有限元建模分析含圆形冲击损伤区的矩形复合材料层板,求解应力及最大位移,并依据最大应力破坏准则,预测复合材料层板的冲击后压缩强度,计算结果与试验数据的比较表明分析结果可靠。