纤维铺层方式对CFRP?铝合金单搭接胶接接头拉伸性能影响

为了分析异质材料胶接接头内部典型应力分布规律与刚度退化特点,探究不同铺层方式对异质材料单搭接胶接接头内部应力分布状态影响规律,开展试验和仿真相关研究。首先,制备不同铺层方式的CFRP（carbon fiber reinforce plastic）?铝合金单搭接胶接接头试验件,使用拉伸试验机进行拉伸试验,获得基本试验数据。其次,利用连续损伤模型、3D Hashin失效判据和Cohesive Zone Model研究异质材料胶接接头不同部位典型破坏特点。结果表明,随着复合材料板中0°铺层比例增加,胶接接头极限载荷呈现增加趋势,与之相反接头拉伸位移逐渐缩短。接头铺层方式与载荷方向共同影响胶接接头力学性能,当复合材料板内部各个方向纤维铺层较为均匀时,可以有效降低接头应力集中,载荷方向与铺层纤维方向一致时,可有效提高接头连接强度。复合材料板中0°铺层占比对接头的极限载荷和刚度退化（scalar stiffness degradation,SDEG）影响较大,0°占比越小接头承载能力越弱,接头刚度退化越复杂。      

圆扇形滑移线场—速度解的校核

滑移线理论是解刚塑性平面应变间题的一种有效方法,而圆扇形场则是常使用的。但求出的速度场与应力场是否一致即λ是否不为负,校核很麻烦。如果不能证明λ≥0,则解的正确性也就得不到证明。本文对圆扇形场进行了分析,并就几种重要的特殊情况得到了具体结果。本文(5)式是从定义直接推出的,也可从文[3]推出。     

利用有限元法分析涡流远场效应的能流通道

涡流远场检测的激励线圈和检测线圈相距较远,两线圈信号相位差对管内壁缺损和管外壁缺损具有相同的灵敏度。传统的涡流理论难以解释涡流远场现象。为了解释涡流远场现象,T.R.Schmidt提出了“能量通道说”,假设检测线圈中的信号是由从激励线圈附近向外穿过管壁再从检测线圈附近向内穿过管壁后的能量激发产生的。本文利用有限元法分析了铁磁性钢管内能量的可能传递途径,结果表明“能量通道说”中的假设是正确的。     

远场应变法测量应力强度因子

本文给出一种将常规电阻应变片贴在距裂纹尖端较远处测量Ⅰ型裂纹应力强度因子K_1的方法。此法实际上是一种实验法与数值法相结合的方法。用实验法测出应变,应变又可以用含待定系数的Williams级数表示,它们组成一组线性代数方程组。解此方程组,可获得待定系数,由待定系数与应力强度因子的已知关系,可求出K_1。 远场应变测量法,避开了裂纹尖端邻域应变梯度很大的区域和可能的塑性区,因而应变测量比较准确。 测出的应变输入数据处理设备及计算机就可以快速实时地知道含裂纹结构在承载情况的K_1,便于进行破坏控制,使设备安全而可靠的工作。     

火星空间磁场低频波动

波动是无碰撞等离子体中能量重新分配的重要途径。对波动的研究有助于更准确地认识太阳风与火星的相互作用,认识火星空间环境的特征。介绍了火星空间中常见的几种磁场低频波动,包括离子回旋波（Ion-CyclotronWave,ICW）、磁流体动力学（MagnetoHydro Dynamic,MHD）波、镜像模波、哨声波以及磁场锯齿状波动,总结了这几类波动的特征和可能的形成机制,说明不同种类的波动所反映的不同的物理过程。由于波粒相互作用在火星离子逃逸的过程中起到了重要作用,波动可影响火星环境的演化。     

木星磁场及磁场模型的对比分析

木星具有太阳系最强的行星磁场,是木星探测面临的基本环境。首先对磁场环境及其数学模型进行了调研,并在研究木星磁场模型以及磁场的数学原理的基础上,使用MATLAB数学工具实现了木星主磁场的计算,对VIP4、VIT4、O6和V1_17ev（eigenvector,特征向量）4个模型与磁测数据进行了对比及分析。研究结果表明这4个模型计算得到的磁场强度范围较为一致,但在全球磁场分布上存在差异,尤其是对磁南极位置的识别上,4个模型的结果都不相同;在对模型计算结果与探测数据的探讨分析中,发现4个模型与探测数据的符合较为一致,偏差均较小。可为木星探测的环境保障提供必要的理论基础和计算模型支撑。     

基于激光反射层析法的换能器声场测量技术及仿真研究

换能器的辐射声场分布能够直接反映出换能器声学性能的好坏,若不能精确测量出换能器的辐射声场,则会对换能器的诊断和评估造成严重影响。从理论仿真的角度出发,推导了运用激光反射层析法重建换能器辐射声场的理论公式,着重利用推导出的理论公式对激光反射层析法进行了仿真计算。结果表明激光反射层析法能够精确地重建出换能器的辐射声场分布及声场中的声压量值,这为换能器的声场重建及声压测量提供了一种可行的方法。     

质子交换炉温度场均匀性分析与优化

针对质子交换炉的温度场均匀性问题,结合质子交换炉的结构特点,基于FLUENT用户自定义函数（UDF）开发了质子交换炉炉温控制算法,并在此基础上提出了多种加热控温方案;利用FLUENT软件对不同方案下的质子交换炉温度场进行仿真,分析不同控温方式下炉内温度场均匀性与传感器位置布置、加热丝布置高度的关系,找到最佳方案。结果表明:采用三段控温、3个传感器位置分别布置在3段加热丝中间、加热丝布置高度4倍于均匀温区长度时炉内温度场均匀性最好,均匀温区内最大偏差为0.03℃;对于既定结构的立式炉体,增加加热丝布置高度、优化设计传感器布置方案和炉体控温方式可以提高温度场均匀性。该方法为同类电加热炉温度场均匀性的优化设计提供了思路。      

A study of a long duration B9 flare-CME event and associated shock

We present and discuss here the observations of a small long duration GOES B-class flare associated with a quiescent filament eruption, a global EUV wave and a CME on 2011 May 11. The event was well observed by the Solar Dynamics Observatory (SDO), GONG H$\alpha$, STEREO and Culgoora spectrograph. As the filament erupted, ahead of the filament we observed the propagation of EIT wave fronts, as well as two flare ribbons on both sides of the polarity inversion line (PIL) on the solar surface. The observations show the co-existence of two types of EUV waves, i.e., a fast and a slow one. A type II radio burst with up to the third harmonic component was also associated with this event. The evolution of photospheric magnetic field showed flux emergence and cancellation at the filament site before its eruption.     

Magnetospheric electric field variations caused by storm-time shock fronts

On January 20, 2005 there was an X 7.1 solar flare at 0636 UT with an accompanied halo coronal mass ejection (CME). The resultant interplanetary shock impacted earth ∼36 h later. Near earth, the Advanced Composition Explorer (ACE) spacecraft observed two impulses with a staircase structure in density and pressure. The estimated earth-arrival times of these impulses were 1713 UT and 1845 UT on January 21, 2005. Three MINIature Spectrometer (MINIS) balloons were aloft on January 21st; one in the northern polar stratosphere and two in the southern polar stratosphere. MeV relativistic electron precipitation (REP) observed by all three balloons is coincident (<3 min) with the impulse arrivals and magnetospheric compression observed by both GOES 10 and 12. Balloon electric field data from the southern hemisphere show no signs of the impulse electric field directly reaching the ionosphere. Enhancement of the balloon-observed convection electric field by as much as 40 mV/m in less than 20 min during this time period is consistent with typical substorm growth. Precipitation-induced ionospheric conductivity enhancements are suggested to be (a) the result of both shock arrival and substorm activity and (b) the cause of rapid (<6 min) decreases in the observed electric field (by as much as 40 mV/m). There is poor agreement between peak cross polar cap potential in the northern hemisphere calculated from Super Dual Auroral Radar Network (SuperDARN) echoes and horizontal electric field at the MINIS balloon locations in the southern hemisphere. Possible reasons for this poor agreement include (a) a true lack of north–south conjugacy between measurement sites, (b) an invalid comparison between global (SuperDARN radar) and local (MINIS balloon) measurements and/or (c) radar absorption resulting from precipitation-induced D-region ionosphere density enhancements.