微颗粒表面磁控溅射镀金属膜实验

采用磁控溅射方法,成功地在微颗粒表面沉积了金属铜膜和金属镍膜.利用光学显微镜(OM)、场发射扫描电子显微镜(FESEM)、能谱仪(EDS)、多功能扫描探针显微镜(SPM)、电感耦合等离子体发射光谱仪(ICP-AES)和光电子能谱仪(XPS)等测试仪器对其表面形貌、膜厚和组份进行了表征.重点讨论了不同的沉积条件对薄膜结晶的影响,并用X射线衍射仪(XRD)对其进行了表征.结果表明,溅射镀膜时,通过控制微颗粒的运动方式,可以在微颗粒表面镀上均匀性好、附着力强和致密性好的金属膜.溅射时间越长或溅射功率越大或装载量越少,都有利于薄膜结晶.      

基于嫦娥一号高能粒子数据的地球磁层屏蔽效应研究

月球绕地球运行轨道约有1/4位于地球磁层内,因此,地球磁层是否会为月球轨道附近高能粒子提供足够的磁场屏蔽对于探索月球活动具有重要影响.嫦娥一号是中国首颗绕月人造卫星,其绕月飞行的工作轨道距离月球表面200 km.通过对嫦娥一号高能粒子探测器(HPD)的探测数据进行分析,比较了当月球位于地球磁层内外6个不同能道(能量范围4～400 MeV)时质子通量的变化,发现当月球位于地球磁层内时,这些能道的质子通量并没有发生显著减少,结果表明地球磁层不能为月球轨道附近高能粒子提供显著的磁屏蔽.     

水流场PIV测试系统示踪粒子特性研究

粒子图像测速技术(PIV)是一种新的流场测量技术,通过对流场中的示踪粒子进行多次曝光成像,获得具有相关性的示踪粒子图像,利用软件对粒子图像进行处理后可得到被测流场的信息.水流场PIV测量利用合适的示踪粒子运动来表征流场状况,示踪粒子的特性对PIV最终测量结果影响很大.讨论了密度、直径、表面反射率等示踪粒子特性对系统实验测量的影响,并特别针对水流场斜入射离轴PIV测试,选择合适的特性参数设计研制了一种简单实用的水流场示踪粒子.通过在直径为100~200μm的聚苯乙烯微球上利用化学方法进行表面镀银,使示踪粒子具有高的光散射特性,实验结果表明这种微粒非常适合于水流场示踪.     

Interfacial characteristics in CNTs-AgCuTi systems

AgCuTi-based composite fillers reinforced with Carbon Nanotubes（CNTs） were prepared by mechanical ball milling and ultrasonic agitation. The morphological features, chemical components, and melting characteristics of the composite fillers with different content of CNTs addition were investigated using Field Emission Scanning Electron Microscopy（FESEM）, XRay Diffraction（XRD） and a Differential Scanning Calorimeter（DSC）. After being heated at 900 ℃, the microstructure of the composite fillers was ...     

旋转对固体火箭发动机两相流点火过程影响仿真研究

为研究高速旋转对内外燃管型装药固体火箭发动机凝聚相点火瞬态过程的影响规律，应用计算流体动力学（CFD）流体计算软件，使用用户定义函数（UDF）编程接口建立固体火箭发动机点火模型，对旋转条件下发动机凝聚相点火过程进行模拟。将数值计算结果与地面旋转实验内弹道进行对比分析，验证数值模型的正确性。计算结果表明：①点火药燃气颗粒因旋转做离心运动，大量粒子聚集在燃烧室头部上端，部分粒子附着在发动机壁面，且停留时间较长。②点火药燃气颗粒占比从20%增加到40%，点火压力峰值降低3.93%，发动机转速的升高会造成内弹道平衡压力升高，但点火压力峰会逐渐降低，且峰值出现时间发生延迟，转速达到15 000 r/min时点火压力峰消失。③转速增大，点火颗粒与推进剂传热增大，火焰传播期减小，但燃气填充期和点火延迟增大，点火药燃气颗粒占比为20%时，转速为15 000 r/min较静止条件下点火延迟增加了23.76%。     

New insights from cross-correlation studies between solar activity indices and cosmic-ray flux during Forbush decrease events

Observed galactic cosmic ray intensity can be subjected to a transient decrease. These so-called Forbush decreases are driven by coronal mass ejection induced shockwaves in the heliosphere. By combining in situ measurements by space borne instruments with ground-based cosmic ray observations, we investigate the relationship between solar energetic particle flux, various solar activity indices, and intensity measurements of cosmic rays during such an event. We present cross-correlation study done using proton flux data from the SOHO/ERNE instrument, as well as data collected during some of the strongest Forbush decreases over the last two completed solar cycles by the network of neutron monitor detectors and different solar observatories. We have demonstrated connection between the shape of solar energetic particles fluence spectra and selected coronal mass ejection and Forbush decrease parameters, indicating that power exponents used to model these fluence spectra could be valuable new parameters in similar analysis of mentioned phenomena. They appear to be better predictor variables of Forbush decrease magnitude in interplanetary magnetic field than coronal mass ejection velocities.