一种新的用于MHD方程逆风格式的Jacobian矩阵分裂方法

针对理想MHD方程,提出了一种新的基于MacCormack算法的雅可比矩阵分裂方法,克服了原有方法稳定性差的问题,并成功地应用于理想MHD方程的求解.控制方程在非结构混合网格上进行空间离散,其中对流项采用本文发展的逆风向量分裂格式,并引入了双曲型磁场散度清除技术,时间推进为显式5步龙格-库塔方法.对MHD激波管流动和带均匀磁场干扰的二维高超声速钝头体绕流流场进行了数值模拟,得到了与参考文献相吻合的数值结果,表明本文发展的数值分裂方法可以有效地捕捉MHD流场的流动特征,并且具有比MacCormack方法更高的稳定性和计算精度.     

非结构网格高超声速化学非平衡MHD流场数值模拟

 在非结构网格上对考虑化学非平衡效应的二维高超声速磁流体绕钝头体流动进行了数值模拟。控制方程由二维理想磁流体动力学（MHD）方程和组元连续方程两部分组成,化学动力学模型为5组元17反应模型。MHD方程空间离散采用AUSM格式,时间推进采用显式5步龙格-库塔格式,并通过弱耦合的方式与化学反应控制方程结合在一起。计算模型为二维钝头体,外加磁场为偶极子场,磁场源位于钝头体内部。在高超声速来流条件下,对有、无磁场干扰,是否考虑化学反应下的4种工况进行了数值计算,得到了满意的结果,并与有限的参考文献进行了对比。结果表明本文发展的方法能准确地模拟考虑化学非平衡效应的高超声速MHD流场。     

NND格式在多维理想磁流体方程组中的应用

采用修正的四步Runge-Kutta方法求解三维一般曲线坐标系下的理想磁流体方程组,为克服数值振荡,加特征型NND格式进行后处理.特征型NND格式推广到求解三维磁流体(MHD)问题需要知道雅可比通量的左右特征矩阵,在具体计算时需要克服矩阵的奇性.本文用三维程序采用推广的特征NND格式计算了一维MHD激波管和二维(MHD)喷管流动,计算结果表明,特征NND格式保持了TVD格式高精度的优点,又具有计算简单的特点,在包括强弱间断等复杂波系的定常和非定常MHD流场数值模拟中是成功的.     

三维磁流体动力学管道流动加减速控制数值研究

阐述了磁流体动力学(MHD)控制流场作用机理.在小磁雷诺数条件下,运用数值模拟方法,对不同外加电磁场条件下三维MHD管道流动的流场情况进行研究,得出不同磁场、电场等MHD参数作用下MHD加速器的性能.对MHD加速器的应用前景进行了展望.计算结果显示,电场取6000V/m,磁场为0.92T 情况下,流场的加速性能可达13.46%,并且可以通过减小磁场或增大电场进一步提高加速性能;在仅添加0.92T磁场条件下,速度减速可达16.35%.     

跨声速压气机数值模拟格式效应研究

针对跨声速叶轮机械复杂内部粘性流动,开发了全三维高精度RANS数值求解器。分别采用FVS格式与AUSM+格式结合多种限制器对Rotor 67跨声速压气机转子进行数值模拟,分析和比较了各格式的计算效果并与试验结果对比。结果表明:与FVS格式相比,AUSM+格式的数值粘性更小,边界层的模拟精度更高;Hemker限制器的综合表现最优,Van Albada限制器的粘性分辨率略低于Hemker限制器,Minmod限制器对流动分离现象的捕捉能力较差,Van Leer限制器容易引入色散误差。     

燃气自由射流的正格式数值模拟

采用二阶正格式方法对复杂燃气自由射流进行了数值模拟。将二维守恒方程的正格式方法发展到轴对称Euler方程组的求解,并对不同欠膨胀压力比下的燃气射流进行了数值计算。计算结果表明,该方法能够较好捕捉到波胞、滑移线、射流边界以及三波点等复杂射流流场波系结构,与实验照片反映的流动特征及高精度、高分辨率的三阶间断有限元方法的计算结果吻合较好,马赫盘位置与理论预估值和实验测量结果误差较小。证明该方法对激波具有较强的捕捉能力,为此类流动的数值研究提供了一种新手段。     

MHD控制激波诱导边界层分离的机理

激波边界层相互作用是高超声速飞行器面临的重大问题,激波入射到平板引起的边界层分离是其中最具代表性的一种。用加权的3阶ENN格式计算了小磁雷诺数近似的MHD方程,研究了MHD控制层流边界层分离的机理。数值结果显示,通过局部电离空气并施加洛伦兹力,能使分离点向下游移动,分离区尺寸减小,从而抑制和缓解由于激波-边界层相互作用而引起的分离。     

超声速主流中横向喷流干扰流场数值模拟

本文用二阶迎风 TVD格式求解层流 N- S方程 ,数值模拟了超声速主流与横向喷流相互作用复杂干扰流场 ,得到了合理的涡系结构 ,计算波系结构及沿物面压力分布也与实验结果一致。计算还表明 ,TVD格式不但具有较强的捕捉激波的能力 ,而且用来模拟复杂涡系结构也是有效的     

自适应的高精度中心﹣WE NO混合格式

为对可压缩流动进行高精度高分辨率的数值模拟,基于模板的光滑度量函数,构造了新型的加权因子,在此基础上将7阶精度的WENO格式与8阶中心格式进行加权组合,构造了一种自适应低耗散的中心-WENO混合格式(H-WENO7-CD8),并采用Fourier方法对离散格式数学特性进行了理论分析。该自适应的高精度中心-WENO混合格式相比于七阶的WENO格式具有更小的耗散误差。通过对激波-密度干扰问题、Rayleigh-Taylor不稳定性问题和双Mach反射问题的数值模拟,并与WENO-JS格式的计算结果对比,结果表明:该格式结合了WENO格式和中心格式的特点,能更好地捕捉激波,对物理脉动也具有较高的分辨率,适合于复杂流体流动的数值模拟。     

振动翼型跨音速绕流的数值模拟

从积分形式的非定常Euler方程出发,在固联于振动冀型的贴体坐标系下,采用有限体积法进行离散,并根据对称型TVD格式构造相应的数值通量,数值模拟了振动翼型的非定常跨音速绕流的变化过程。计算结果表明,该方法能较好地捕捉流场中的运动激波,准确地定出激波位置与强度;并且易于推广到求解任意振动方式的跨音速非定常绕流问题。     

MHD ANALYSIS OF PETSCHEK-TYPE RECONNECTION IN NON-UNIFORM FIELD AND FLOW GEOMETRIES

Analytical studies of reconnection have, for the most part, been confined to steady and uniform current sheet geometries. In contrast to these implifications, natural phenomena associated with the presence of current sheets indicate highly non-uniform structure and time-varying behaviour. Examples include the violent outbursts of energy on the Sun known as solar flares, and magnetospheric phenomena such as flux transfer events, plasmoids, and auroral activity. Unlike the theoretical models, reconnection therefore occurs in a highly dynamic and structured plasma environment. In this article we review the mathematical tools and techniques which are available to formulate models capable of describing the effects of reconnection in such situations. We confine attention to variants of the reconnection model first discussed by Petschek in the 1960s, in view of its successful application in predicting and interpreting phenomena in the terrestrial magnetosphere. The analysis of Petschek-type reconnection is based on the equations of ideal magnetohydrodynamics (MHD), which describe the large-scale behaviour of the magnetic field and plasma flow outside the diffusion region, which we determine as a localised part of the current sheet in which reconnection is initiated. The approach we adopt here is to transform the MHD equations into a Lagrangian or so-called 'frozen-in' coordinate system. In this coordinate system, the equation of motion transforms into a set of coupled nonlinear equations, in which the presence of inhomogeneous magnetic fields and/or plasma flows gives rise to a term similar to that which appears in the study of the ordinary string equation in a non-homogeneous medium. As demonstrated here, this approach not only clarifies and highlights the effects of such non-uniformities, it also simplifies the solution of the original set of MHD equations. In particular, this is true for those types of problem in which the total pressure can be considered as a known quantity from the outset. To illustrate the method, we solve several 2D problems involving magnetic field and flow non-uniformities: reconnection in a stagnation-point flow geometry with antiparallel magnetic fields; reconnection in a Y-type magnetic field geometry with and without velocity shear across the current sheet; and reconnection in a force-free magnetic field geometry with field lines of the form xy = const. These case examples, chosen for their tractability, each incorporate some aspects of the field and flow geomtries encountered in solar-terrestrial applications, and they provide a starting point for further analytical as well as numerical studies of reconnection.     

A Class of TVD Type Combined Numerical Scheme for MHD Equations With a Survey About Numerical Methods in Solar Wind Simulations

It has been believed that three-dimensional, numerical, magnetohydrodynamic (MHD) modelling must play a crucial role in a seamless forecasting system. This system refers to space weather originating on the sun; propagation of disturbances through the solar wind and interplanetary magnetic field (IMF), and thence, transmission into the magnetosphere, ionosphere, and thermosphere. This role comes as no surprise to numerical modelers that participate in the numerical modelling of atmospheric environments as well as the meteorological conditions at Earth. Space scientists have paid great attention to operational numerical space weather prediction models. To this purpose practical progress has been made in the past years. Here first is reviewed the progress of the numerical methods in solar wind modelling. Then, based on our discussion, a new numerical scheme of total variation diminishing (TVD) type for magnetohydrodynamic equations in spherical coordinates is proposed by taking into account convergence, stability and resolution. This new MHD model is established by solving the fluid equations of MHD system with a modified Lax-Friedrichs scheme and the magnetic induction equations with MacCormack II scheme for the purpose of developing a combined scheme of quick convergence as well as of TVD property. To verify the validation of the scheme, the propagation of one-dimensional MHD fast and slow shock problem is discussed with the numerical results conforming to the existing results obtained by the piece-wise parabolic method (PPM). Finally, some conclusions are made. This revised version was published online in August 2006 with corrections to the Cover Date.     

Alfvén wave heating

This review discusses Alfvén wave heating in non-uniform plasmas as a possible means for explaining the heating of the solar corona. It focusses on recent analytical results that enable us to understand the basic physics of Alfvén wave heating and help us with the interpretation of results of numerical simulations. First we consider the singular wave solutions that are found in linear ideal MHD at the resonant magnetic surface where the frequency of the wave equals the local Alfvén frequency. Next, we use linear resistive MHD for describing the waves in the dissipative region and explain how dissipation modifies the singular solutions found in linear ideal MHD.     

A Parallel Adaptive 3D MHD Scheme for Modeling Coronal and Solar Wind Plasma Flows

A parallel adaptive mesh refinement (AMR) scheme is described for solving the governing equations of ideal magnetohydrodynamics (MHD) in three space dimensions. This solution algorithm makes use of modern finite-volume numerical methodology to provide a combination of high solution accuracy and computational robustness. Efficient and scalable implementations of the method have been developed for massively parallel computer architectures and high performance achieved. Numerical results are discussed for a simplified model of the initiation and evolution of coronal mass ejections (CMEs) in the inner heliosphere. The results demonstrate the potential of this numerical tool for enhancing our understanding of coronal and solar wind plasma processes. This revised version was published online in June 2006 with corrections to the Cover Date.     

Modelling of Solar Wind, CME Initiation and CME Propagation

Simulations of coronal mass ejections (CMEs) evolving in the interplanetary (IP) space from the Sun up to 1 AU are performed in the framework of ideal magnetohydrodynamics (MHD) by the means of a finite-volume, explicit solver. The aim is to quantify the effect of the background solar wind and of the CME initiation parameters, such as the initial magnetic polarity, on the evolution and on the geo-effectiveness of CMEs. First, three different solar wind models are reconstructed using the same numerical grid and the same numerical scheme. Then, different CME initiation models are considered: Magnetic foot point shearing and magnetic flux emergence. For the fast CME evolution studies, a very simple CME model is considered: A high-density and high-pressure magnetized plasma blob is superposed on a background steady state solar wind model with an initial velocity and launch direction. The simulations show that the initial magnetic polarity substantially affects the IP evolution of the CMEs influencing the propagation velocity, the shape, the trajectory (and thus, the geo-effectiveness).     

3D nonlinear wave heating of coronal loops

The heating of solar coronal loops by the resonant absorption or phase-mixing of incident wave energy is investigated in the framework of 3D nonlinear magnetohydrodynamics (MHD) by means of numerical simulations.