MHD控制激波诱导湍流边界层分离的机理分析

为了研究磁流体动力学(Magnetohydrodynamics:MHD)加速边界层对激波-湍流边界层相互作用的影响,用高阶有限差分法求解了小磁雷诺数近似的MHD湍流方程。其中,无粘通量采用WENN格式离散、粘性通量采用Roe平均中心差分离散,时间采用半隐式推进,并采取追赶法求解。计算给出了湍流、电场、磁场和电导率等参数对边界层分离的影响,数值结果显示:在同样的逆压梯度下,湍流边界层分离能更快地趋于稳态流场,且分离区比层流小;通过施加洛仑兹力加速,边界层速度型面变得更加饱满、位移厚度减小、分离点和再附点向激波与固壁的交点靠近,分离区尺寸减小甚至最终被消除。     

基于电子束电离的磁流体力学进气道流动控制数值模拟

采用基于电子束电离的磁流体力学(MHD)控制系统,对高超声速流场附面层,以及非设计状态下的高超声速进气道流场的磁流体控制进行了深入研究.控制方程为低磁雷诺数Navier-Stokes方程,采用等离子体动力学模型与电子束模型模拟空气电离过程.研究结果表明:①电子束电离能有效提高流场的电导率,增强磁场对流场的控制效率;②基于电子束诱导电离的MHD控制系统能有效地控制高超声速流场的附面层,但其控制效率跟电子束能量大小相关;③基于电子束诱导电离的MHD控制系统能有效地改变非设计状态下高超声速飞行器的斜激波结构,使进气道重新满足Shock-on-lip(SOL)条件,但进气道的总压恢复系数以及流量将会降低.      

三维磁流体强化超燃冲压发动机数值模拟

建立了三维磁流体强化超燃冲压发动机内部黏性流场的求解模型.针对马赫数为6设计了联合应用磁控进气道和磁流体能量旁路的磁流体强化超燃冲压发动机模型.针对该模型进行了数值模拟研究,分析其中的三维流场结构、电参数分布规律以及能量转换特性.结果表明:当飞行马赫数为8时,磁控进气道的应用能够使头部压缩激波回到唇口,使分离区消失,内进气道中的流动恢复到设计状态.磁流体能量旁路可有效降低燃烧室入口处的马赫数,从而改善发动机性能.其中发生器中的流动参数和电参数的分布比较理想,效果显著;而加速器要取得显著的加速效果则需要大量的能量输入.在加速器中,电极附近焦耳耗散严重,导致局部高温以及流动的复杂性,性能不够理想.      

方腔流致振荡及噪声的数值研究

采用直接数值模拟方法,研究了低Reynolds数下L/D=2的方腔亚声速流致振荡现象及其诱导的噪声。结果表明,在所计算的参数范围内,振荡都是由Rossiter II模态主导;来流边界层变薄会导致低频成分的出现,其产生的直接原因是涡与后拐角撞击方式的切换,根源在于回流区与剪切层相互作用形式的不稳定。采用本征正交分解(POD)方法,分析了不同振荡形式所对应的本征模态涡结构及其与后拐角撞击方式的关系。计算得到并分析了声波的产生和传播过程,结果与已有实验结果和理论模型符合良好。     

电导率模拟对高超声速MHD控制影响

高温气体电导率是高超声速电磁流动控制数值模拟最重要的参数之一。针对电导率模拟准确性及其对高超声速磁流体控制影响的问题,考虑高超声速飞行器流场中高温气体热化学非平衡效应,采用三维低磁雷诺数磁流体动力学（MHD）数值模拟方法及程序,结合国内外常见电导率处理方法开展典型状态高超声速MHD控制数值模拟,分析电导率模拟对高超声速磁流体流场分布、气动力/热特性的影响。研究表明：磁控热流减缓效果与电导率呈非线性关系,电导率较大时将出现电导率的磁控热饱和现象,其产生的原因可能与化学反应趋向于平衡态存在一定关系;采用定电导率方法,会人为放大磁场洛仑兹力的磁阻力效果,使阻力系数的预测值偏大;不同电导率模型计算得到的电导率分布差异很大,甚至存在数量级的差别,显著影响了磁流体的控制效果,这与电导率模型的适用范围、参数选取原则存在很大关联;对于含多种离解、电离组分的高温气体流动来说,采用基于多电离组分迁移碰撞的电导率模型（本文模型M8）,计算与试验一致性最好。     

三角翼前缘涡破裂点脉动的实验分析

在水槽中和风洞中分别进行了流动显示和动态测压实验,目的是研究三角翼前缘涡破裂点的脉动现象.对流动显示图片中涡的破裂点位置进行统计和频谱分析,表明破裂点振荡存在双主频特征,位于0.07位置的主频对应着螺旋—泡—螺旋的转化过程,位于0.2~0.4之间的主频对应着螺旋形态破裂本身的小幅振动.对统计的破裂点位置数据做低通滤波后进行相关性分析,还表明了三角翼左右2个前缘涡的破裂点位置信号具有负相关性.进行三角翼表面动态压力测量,对压力数据低通滤波后做相关性分析,发现相同的一条前缘涡的动态压力信号在整个翼面上都具有高度的相关性.      

Two energy release processes for CMEs: MHD catastrophe and magnetic reconnection

It remains an open question how magnetic energy is rapidly released in the solar corona so as to create solar explosions such as solar flares and coronal mass ejections (CMEs). Recent studies have confirmed that a system consisting of a flux rope embedded in a background field exhibits a catastrophic behavior, and the energy threshold at the catastrophic point may exceed the associated open field energy. The accumulated free energy in the corona is abruptly released when the catastrophe takes place, and it probably serves as the main means of energy release for CMEs at least in the initial phase. Such a release proceeds via an ideal MHD process in contrast with nonideal ones such as magnetic reconnection. The catastrophe results in a sudden formation of electric current sheets, which naturally provide proper sites for fast magnetic reconnection. The reconnection may be identified with a solar flare associated with the CME on one hand, and produces a further acceleration of the CME on the other. On this basis, several preliminary suggestions are made for future observational investigations, especially with the proposed Kuafa satellites, on the roles of the MHD catastrophe and magnetic reconnection in the magnetic energy release associated with CMEs and flares.     

Characterization of the slow wind in the outer corona

The study concerns the streamer belt observed at high spectral resolution during the minimum of solar cycle 23 with the Ultraviolet Coronagraph Spectrometer (UVCS) onboard SOHO. On the basis of a spectroscopic analysis of the O VI doublet, the solar wind plasma parameters are inferred in the extended corona. The analysis accounts for the coronal magnetic topology, extrapolated through a 3D magneto-hydrodynamic model, in order to define the streamer boundary and to analyse the edges of coronal holes. The results of the analysis allow an accurate identification of the source regions of the slow coronal wind that are confirmed to be along the streamer boundary in the open magnetic field region.     

Simulation of the observed coronal kink instability and its implications for the SDO/AIA

Srivastava et al. (2010) have observed a highly twisted coronal loop, which was anchored in AR10960 during the period 04:43 UT-04:52 UT on 4 June 2007. The loop length and radius are approximately 80 Mm and 4 Mm, with a twist of 11.5 π$\pi$. These observations are used as initial conditions in a three dimensional nonlinear magnetohydrodynamic simulation with parallel thermal conduction included. The initial unstable equilibrium evolves into the kink instability, from which synthetic observables are generated for various high-temperature filters of SDO/AIA. These observables include temporal and spatial averaging to account for the resolution and exposure times of SDO/AIA images. Using the simulation results, we describe the implications of coronal kink instability as observables in SDO/AIA filters.