Theoretical model of steady-state magnetic reconnection in collisionless incompressible plasma based on the Grad–Shafranov equation solution

The problem of steady-state magnetic reconnection in an infinite current layer in collisionless, incompressible, nonresistive plasma, except of the electron diffusion region, is examined analytically using the electron Hall magnetohydrodynamics approach. It is found that this approach allows reducing the problem to the magnetic field potential finding, while last one has to satisfy the Grad–Shafranov equation. The obtained solution demonstrates all essential Hall reconnection features, namely proton acceleration up to Alfvén velocities, the forming of Hall current systems and the magnetic field structure expected. It turns out that the necessary condition of steady-state reconnection to exist is an electric field potential jump across the electron diffusion region and the separatrices. Besides, the powerful mechanism of electron acceleration in X-line direction is required. It must accelerate electrons up to the electron Alfvén velocity inside the diffusion region and on the separatrixes. This is a necessary condition for steady-state reconnection as well.     

MHD oscillations in solar and stellar coronae: Current results and perspectives

Wave and oscillatory activity is observed with modern imaging and spectral instruments in the visible light, EUV, X-ray and radio bands in all parts of the solar corona. Magnetohydrodynamic (MHD) wave theory gives satisfactory interpretation of these phenomena in terms of MHD modes of coronal structures. The paper reviews the current trends in the observational study of coronal oscillations, recent development of theoretical modelling of MHD wave interaction with plasma structures, and implementation of the theoretical results for the mode identification. Also the use of MHD waves for remote diagnostics of coronal plasmas is discussed. In particular, the applicability of this method to the estimation of the coronal magnetic field is demonstrated.     

磁流体发电系统在空间电源中的应用研究

介绍了直线型和盘式磁流体(MHD)发电机,鉴于盘式磁流体发电机结构紧凑、发电效率高、对应磁体系统简单等优点,建议在大型航天器上采用盘式磁流体发电机。根据空间应用的特点,盘式磁流体发电机的工质应选用氦/氙混合气体;在抑制等离子体的不稳定时,应综合使用扩张通道、导流片、波状外形壁面及射频线圈等方法。对空间盘式磁流体发电系统及试验设备研究情况进行了介绍;以高温气体闭环核能磁流体发电系统为例,分析了其工作原理和质量功率比等性能参数;总结出地面试验的研究趋势是向超长时间运行发展。针对我国在反应堆、材料、工艺等方面的发展现状,建议深入开展磁流体发电技术及盘式磁流体发电机研究,突破等离子体参数测量、稳定性等关键技术,促进我国在空间核动力技术领域的快速发展。     

Solar Nebula Magnetohydrodynamics

The dynamical state of the solar nebula depends critically upon whether or not the gas is magnetically coupled. The presence of a subthermal field will cause laminar flow to break down into turbulence. Magnetic coupling, in turn, depends upon the ionization fraction of the gas. The inner most region of the nebula (≲0.1 AU) is magnetically well-coupled, as is the outermost region (≳10 AU). The magnetic status of intermediate scales (∼1 AU) is less certain. It is plausible that there is a zone adjacent to the inner disk in which turbulent heating self-consistently maintains the requisite ionization levels. But the region adjacent to the active outer disk is likely to be magnetically ``dead.' Hall currents play a significant role in nebular magnetohydrodynamics. Though still occasionally argued in the literature, there is simply no evidence to support the once standard claim that differential rotation in a Keplerian disk is prone to break down into shear turbulence by nonlinear instabilities. There is abundant evidence—numerical, experimental, and analytic—in support of the stabilizing role of Coriolis forces. Hydrodynamical turbulence is almost certainly not a source of enhanced turbulence in the solar nebula, or in any other astrophysical accretion disk. This revised version was published online in June 2006 with corrections to the Cover Date.     

绕流圆柱的自由表面磁流体流动实验

利用PIV(Particle image velocimetry)光学测量系统,在雷诺数分别为7 767和11 60时,实验研究了磁场对绕流圆柱的自由表面流动的影响.实验研究结果表明,磁场使边界层内的无量纲平均速度分布偏离对数分布,尾迹变窄变短,分离点向后移;当雷诺数增加到11 60时,在相同磁场强度作用下,磁场的影响减弱,从而使边界层内的无量纲平均速度分布偏离对数分布的程度减小.      

含不确定参数的复合材料壁板热颤振分析

研究了含有不确定结构参数的壁板颤振问题,利用vonKarman大变形应变-位移关系、气动力活塞理论和准定常热应力理论建立了复合材料壁板颤振的气动弹性力学模型,考虑在壁板颤振分析模型中存在的不确定参数,将其用区间向量定量化,基于区间扩张理论和Taylor级数展开,并结合有限元计算方法,提出了区间分析的方法来估计含有不确定参数的壁板结构颤振临界风速的区间,以及发生极限环振动时振幅的变化区间。通过数值算例,将本文提出的壁板颤振的区间有限元模型与随机有限元模型进行了比较,显示了本文方法的有效性和可行性。这种方法的优点是只需要知道不确定参数的所在范围界限,为解决含有不确定参数的壁板颤振这类复杂的气动弹性动力学问题提供了一个途径。     

超燃冲压发动机磁控进气道设计影响因素分析

阐述了磁控进气道的基本原理,建立了一维数学模型。对磁控进气道设计影响因素磁感应强度、负载系数和通道截面积变化率进行了特性分析,得到磁控进气道出口参数随设计参数的变化规律,为磁控进气道设计提供了依据。给出了一组磁控进气道设计参数,仿真结果表明采用磁控进气道技术可以有效地调节燃烧室进口来流状态,提高比冲,拓宽飞行马赫数范围。      

各向异性磁流体激波跃变关系的无量纲化求解

用无量纲化方法，推出了各向压力异性等离子体中磁流体激波跃变条件及其解析解的一种普遍而简单的形式，并讨论了它在各向同性等离子体中各种特殊情况下的结果．     

非定常N－S方程的线化及其差分求解

在微幅简谐振荡的假设下，对计算平面内非定常Ｎ－Ｓ方程进行了线比，并在ＭａｃＣｏｒｍａｒｋ于１９８０年提出的半隐格式的基础上，发展了一种适用于求解计算平面内线化Ｎ－Ｓ方程的差分格式．用该差分格式求解计算平面内的线化Ｎ－Ｓ方程时，可以避免求解五对角方程；且时间步长可以取得较大，计算效率高．