无机粒子对石墨烯微片／环氧树脂复合材料导电性能的影响

以 KNG-CZ030石墨烯（graphene nanoplatelets,GNPs）为导电填料,环氧树脂（E-54）为聚合物基体,2-乙基-4甲基咪唑（2,4-EMI）为固化剂,采用溶液混合和超声分散的方法制备导电复合材料。通过添加无机粒子（NaCl, TiO2）,研究了无机粒子对石墨烯微片分散均匀性的影响以及对 GNPs ／E-54复合材料导电性能的影响。实验结果表明：加入 NaCl 和 TiO2提高了石墨烯微片在基体中的分散性,降低了复合材料室温体积电阻率,即提高了导电性能;NaCl ／GNPs ／E-54和 TiO2／GNPs ／E-54复合材料室温体积电阻率为106Ω·m 时,石墨烯质量分数分别为0．75％和0．73％,与未添加无机粒子的 GNPs ／E-54复合材料质量分数0．97％相比有所降低。     

航空发动机滑油颗粒监测与控制标准研究

在航空发动机零部件的加工、装配及发动机工厂试车和检验试车过程中,运用先进的技术手段,开展以发动机零部件清洁度控制、装配清洁度控制及试车阶段滑油磨粒的监测试验,探索滑油中污染物的来源、污染程度及其对发动机使用的影响,确定磨粒来源、产生原因及典型故障模式,提出减少、控制污染物及磨粒的改进意见,进而制定出发动机滑油颗粒监测与控制标准,并应用于发动机生产及零部件的质量控制,对改进产品质量,降低生产成本,缩短生产周期等具有重要意义。     

基于UPF的航天器自主天文导航方法

利用红外地球敏感器和星敏感器直接敏感地平的天文导航方法是一种成熟、可靠的自主导航方法。这种导航方法的状态方程和量测方程都是严重非线性的,且在建立航天器轨道动力学模型时,通常将二阶带谐摄动项建模,而将其他摄动项等效为高斯白噪声,由于这些摄动项都有其精确的模型,通常不服从高斯分布。本文提出将UPF(Unscented Particle Filter)滤波方法应用于航天器自主天文导航,该方法用UKF(Unscented Kalman Filter)得到粒子滤波的重要性采样密度函数,从而克服了标准的粒子滤波没有考虑最新量测信息和UKF只能应用于噪声为高斯分布的不足。仿真结果表明,该方法可以取得比标准的粒子滤波和UKF更快的滤波收敛性和更高的滤波精度。     

应用双镜头三维 LDV/PDPA 系统诊断液流模型流动特性方法

在双透镜模式三维激光测速系统的基础上,提出了在测量液体模型时修正入射光聚焦变形的光程角－位移补偿法。此方法使两个入射透镜的入射光在具有多层不同性质介质的模型中保持相交,并通过位移补偿使入射光相交在同一测量平面上,得到了与入射角、介质折射率及坐标架位移有关的补偿公式。利用实时三维ＰＤＰＡ系统对旋转水流模型进行了调整和测量,实验结果证明了该方法的原理是正确的,对解决不同折射率介质的液体流场及液－固、液－气两相流等流场特性的测量中存在的问题是可行的。     

富燃料推进剂燃烧产物粒度参数的激光衰减法测量

介绍了激光衰减法测量粒子参数的基本原理.搭建了激光衰减法测量高铝含量富燃料推进剂实验系统,解决了燃烧环境下粒度测试的光学介入问题,对高铝含量富燃料推进剂中粒子参数进行测量,对所得的凝相燃烧产物进行电镜分析,并对电镜照片进行分析处理,计算出燃烧后凝相产物平均粒径,验证了激光衰减法测量粒子参数的可行性和合理性.     

无网格SPH法中守恒光滑法的修正

守恒光滑法CSA(Conservative Smoothing Approach)是解决传统SPH(Smoothed Particle Hydrodynamics)法稳定性问题的一种很有效的方法.研究发现在SPH法中运用所谓的守恒光滑法并不能保证系统的总物理量(质量、动量或者能量)在每个时间步均守恒,而是随着时间在理论值附近波动,对计算结果的精度有一定的影响.对此提出了守恒光滑法的修正公式,对SPH控制方程得到的各个粒子的物理量进行CSA光滑,然后运用文中提出的CSA的修正公式把对该粒子物理量的改变量加权平均给邻域内各个粒子,从而确保了SPH算法中系统的总物理量(质量、动量以及能量等)在每个时间步均守恒,而且由于减少了CSA对SPH得到的各个粒子物理量的过分光滑,从而提高了计算精度.物理意义、理论推导以及文中的算例均证明了这种修正的有效性.     

Physics of ion acceleration in the solar flare on 2005 September 7 determines γ-ray and neutron production

Relativistic neutrons were observed by the neutron monitors at Mt. Chacaltaya and Mexico City and by the solar neutron telescopes at Chacaltaya and Mt. Sierra Negra in association with an X17.0 flare on 2005 September 7. The neutron signal continued for more than 20 min with high statistical significance. Intense emissions of γ-rays were also registered by INTEGRAL, and during the decay phase by RHESSI. We analyzed these data using the solar-flare magnetic-loop transport and interaction model of Hua et al. [Hua, X.-M., Kozlovsky, B., Lingenfelter, R.E. et al. Angular and energy-dependent neutron emission from solar flare magnetic loops, Astrophys. J. Suppl. Ser. 140, 563–579, 2002], and found that the model could successfully fit the data with intermediate values of loop magnetic convergence and pitch-angle scattering parameters. These results indicate that solar neutrons were produced at the same time as the γ-ray line emission and that ions were continuously accelerated at the emission site.     

Solar wind low-energy energetic ion enhancements: A tool to forecast large geomagnetic storms

Predicting the occurrence of large geomagnetic storms more than an hour in advance is an important, yet difficult task. Energetic ion data show enhancements in flux that herald the approach of interplanetary shocks, usually for many hours before the shock arrival. We present a technique for predicting large geomagnetic storms (Kp  7) following the arrival of interplanetary shocks at 1 AU, using low-energy energetic ions (47–65 keV) and solar wind data measured at the L1 libration point. It is based on a study of the relationship between energetic ion enhancements (EIEs) and large geomagnetic storms by Smith et al. [Smith, Z., Murtagh, W., Smithtro, C. Relationship between solar wind low-energy energetic ion enhancements and large geomagnetic storms. J. Geophys. Res. 109, A01110, 2004. doi:10.1029/ 2003JA010044] using data in the rise and maximum of solar cycle 23 (February 1998–December 2000). An excellent correlation was found between storms with Kp  7 and the peak flux of large energetic ion enhancements that almost always (93% of time in our time period) accompany the arrival of interplanetary shocks at L1. However, as there are many more large EIEs than large geomagnetic storms, other characteristics were investigated to help determine which EIEs are likely to be followed by large storms. An additional parameter, the magnitude of the post-shock total magnetic field at the L1 Lagrangian point, is introduced here. This improves the identification of the EIEs that are likely to be followed by large storms. A forecasting technique is developed and tested on the time period of the original study (the training data set). The lead times, defined as the times from the arrival of the shock to the start of the 3-h interval of maximum Kp, are also presented. They range from minutes to more than a day; the average for large storms is 7 h. These times do not include the extra warning time given when the EI flux cross the high thresholds ahead of the shock. Because the data-stream used in the original study is no longer available, we extended the original study (1998–2000) to 2001, in order to: (a) investigate EIEs in 2001; (b) present a validation of the technique on an independent data set; (c) compare the results based on the original (P1) energy channel to those of the replacement (P1′) and (d), determine new EIE thresholds for forecasting geomagnetic storms using P1′ data. The verification of this P1′ training data set is also presented, together with lead times.     

基于社会模型改进粒子群算法的翼型优化设计

为了解决粒子群算法在寻优过程中全局最优和局部最优的矛盾,通过在粒子群算法优化过程中引入鱼类的聚群行为,发展了一种基于社会模型的改进粒子群算法。算法以粒子可视范围的不同用法为基础,提出了两种不同的优化策略,同时探讨了种群规模等参数对算法性能的影响,并通过函数测试结果证明了两种优化策略的有效性和不同的优化特性。将改进的优化算法应用在翼型的气动优化中,显著改善了翼型气动特性,提高了算法的全局搜索能力,取得了良好的优化效果。     

粒子分离器叶片涂层冲蚀磨损的数值模拟

以叶片涂层为对象,研究其冲蚀过程中损伤的演化过程.首先进行了流场计算.其次通过对单个固体颗粒冲蚀过程的模拟,提出了"碰撞有效影响区域"的概念,使得多个固体颗粒连续冲蚀数值模拟得以实现.接下来通过模拟"碰撞有效影响区域"内材料受到固体颗粒连续冲蚀的过程获得材料的抗冲蚀磨损性能.最后,将流场数据和涂层抗冲蚀磨损性能参数相结合来模拟叶片涂层的冲蚀过程,指出了涂层的薄弱区域并进行了寿命预测.