模拟弹塑性碰撞的修正SPH方法

从基本的无网格光滑粒子法SPH(Smoothed Particle Hydrodynamics)近似出发,修正了模拟固体力学中大变形弹塑性碰撞的SPH方法.在边界处采用修正的边界条件,弹塑性分析过程中采用增量理论计算应力,迭代过程中用守恒光滑法进行滤波修正消除拉力不稳定.对SPH方法进行了程序实现,给出了杆弹塑性碰撞的算例.计算分析表明,SPH方法节点的影响域较大、精度较相同节点间距有限元法的结果有一定差距,但是通过增加粒子数量可以提高SPH的精度,保持了其简单性和计算大变形的特性.      

单激励直线行波超声马达定子振动特性研究

利用弹性动力学理论对半无限长弹性细长梁进行了分析,得出在弹性细长梁上激励出大振幅弯曲行波振动的条件,对以此为基础研制的直线超声行波马达的定子进行了振动特性分析,着重分析了行波反射对定子振动状态的影响,认为一般情况下定子上的振动是含有驻波场的行波,并对不同反射系数条件下的定子振动波形进行仿真,最后通过实验研究了驻波场对超声马达驱动特性的影响.      

正弦波型高频动态压力光学校准系统及其应用

动态压力是气动部件表面的关键气动参数。光学压力敏感涂料（PSP）测量技术在测量气动部件表面动态压力方面具有全域测量、不影响流场自身的优势，而光学压力敏感涂料的动态响应特性则是进行动态压力测量的决定性因素。基于声学驻波管原理，自主设计并组建了正弦波型高频动态压力光学校准系统，主要包含有驻波管型校准舱、声源、激光源、高频压力传感器、光电倍增管以及测控系统。对动态压力光学校准系统及某新型快响压敏涂料的实验结果表明，所组建的动态压力校准系统可产生最短响应时间12.5 μs、最大压力幅值为4.37 kPa的正弦型动态压力，其有效动态频响范围为0.4~20.0 kHz（50 μs~2.5 ms），不确定度小于0.004 9%；校准系统合理的光路布局可进行快响压敏涂料动态特性的校准，所测涂料可用于动态频响不高于9.1 kHz（响应时间为109.9 μs）的非定常流场的压力测量。     

基于SPH的小型飞机水上迫降姿态数值仿真

适航条例中要求飞机必须具备良好的水上迫降性能。早期主要通过试验方法研究飞机的水上迫降性能,但是试验耗资巨大、时间周期长。采用一种新型的数值模拟方法研究飞机水上迫降问题,利用光滑质点流体动力学(SPH)方法模拟三级波浪,建立小型飞机水上迫降模型。考虑到飞机姿态角和起落架收放状态对迫降性能的影响,建立7种计算工况,模拟得到相应的加速度响应和姿态角变化。以飞机在迫降过程中应该受到较小的加速度响应和姿态角变化为依据,通过对比分析计算结果,最终给出12°姿态角、起落架收起为最优迫降状态的结论,为飞机迫降的入水姿态提供技术支持。     

内置开孔隔墙的高速铁路隧道压力波数值模拟方法

基于一维可压缩非定常不等熵流动模型、薄壁孔口出流模型以及广义黎曼变量特征线法,发展了单列车通过内置开孔隔墙隧道的压力波数值分析方法.与国外试验结果比较验证本文建立的计算方法的正确合理性基础上,通过对不同开孔率的计算得出采用过大的开孔率将导致一维流动模型计算时出现较大的数值振荡,分析了计算结果震荡可能的—维流动模型适用性的原因.同时,通过对隔墙中开孔和不开孔的模拟计算,得出隔墙开孔可较大幅度的减缓压力波,为今后研究和隧道内设置开孔隔墙提供了有益的启示.     

消除粘性项高阶离散数值振荡的半结点-结点交错方法

通常的粘性项处理方法是连续两次采用结点型中心差分格式求得.但是,通过两次采用高阶结点型中心格式求得的粘性项易在流场中的"间断"附近产生数值振荡.本文采用多种格式,通过求解一维Burgers方程来充分展示了这种振荡现象.为了消除这种数值振荡,一种半结点型的高阶紧致格式被用来求解粘性项.Fourier频谱分析表明,这种格式具有非常优越的保频谱性能.一维和二维的数值计算结果表明,通过"半结点-结点"交错采用这种半结点型格式的方法可以非常有效地避免粘性项高阶离散可能导致的数值振荡.     

环形射流喷口位置对激波聚焦起爆的影响分析

为了研究环形射流喷口位置对激波聚焦起爆爆震的影响,以氢气和空气混合物为例,对不同环形射流喷口位置条件下的激波聚焦起爆过程进行了数值模拟。结果表明,随着喷口距凹壁面距离L增大,直接聚焦起爆和凹壁面反射起爆所需的临界入射压力逐渐增大,相应的聚焦时刻会滞后,形成焦点的位置距凹壁面越远。     

Effects of adiabaticity and non-adiabaticity of dust charge fluctuation on the propagation of the dust ion acoustic waves in inhomogeneous dusty plasma

A theoretical investigation has been made for adiabatic positive and negative dust charge fluctuations on the propagation of dust-ion acoustic waves (DIAWs) in a weakly inhomogeneous, collisionless, unmagnetized dusty plasmas consisting of cold positive ions, stationary positively and negatively charged dust particles and isothermal electrons. The reductive perturbation method is employed to reduce the basic set of fluid equations to the variable coefficients Korteweg–de Vries (KdV) equation. Either compressive or rarefactive solitons are shown to exist depending on the critical value of the ion density, which in turn, depends on the inhomogeneous distribution of the ion. The dissipative effects of non-adiabatic dust charge variation has been studied which cause generation of dust ion acoustic shock waves governed by KdV-Burger (KdVB) equation. The results of the present investigation may be applicable to some dusty plasma environments, such as dusty plasma existing in polar mesosphere region.     

Ion- and electron-acoustic solitons and double layers in multi-component space plasmas

A general model for the ion- and electron-acoustic solitons and double layers in a multi-component unmagnetized plasma consisting of background electrons, counter-streaming electron beams and ions is discussed. The model is based on the multi-fluid equations and the Poisson equation, and uses the Sagdeev pseudo-potential techniques. For identical counter-streaming electron beams and depending upon the plasma parameters, three types of solutions, namely, ion-acoustic, slow and fast electron-acoustic soliton/double layer, are possible. Generally, the ion acoustic solitons have positive potentials, slow-electron acoustic solitons have negative potentials and fast electron-acoustic solitons and double layers can have either positive or negative potentials depending on the core electron density. As beam speed is increased, first ion-acoustic and then slow electron-acoustic solitons disappear. At large beam speed, only fast electron-acoustic solitons/double layers survive. The results may be relevant to the observations of the electrostatic solitary waves (ESWs) observed in the Earth’s magnetosphere.     

Cosmological Shock Waves

Large-scale structure formation, accretion and merging processes, AGN activity produce cosmological gas shocks. The shocks convert a fraction of the energy of gravitationally accelerated flows to internal energy of the gas. Being the main gas-heating agent, cosmological shocks could amplify magnetic fields and accelerate energetic particles via the multi-fluid plasma relaxation processes. We first discuss the basic properties of standard single-fluid shocks. Cosmological plasma shocks are expected to be collisionless. We then review the plasma processes responsible for the microscopic structure of collisionless shocks. A tiny fraction of the particles crossing the shock is injected into the non-thermal energetic component that could get a substantial part of the ram pressure power dissipated at the shock. The energetic particles penetrate deep into the shock upstream producing an extended shock precursor. Scaling relations for postshock ion temperature and entropy as functions of shock velocity in strong collisionless multi-fluid shocks are discussed. We show that the multi-fluid nature of collisionless shocks results in excessive gas compression, energetic particle acceleration, precursor gas heating, magnetic field amplification and non-thermal emission. Multi-fluid shocks provide a reduced gas entropy production and could also modify the observable thermodynamic scaling relations for clusters of galaxies.