Eruptive prominences as sources of magnetic clouds in the solar wind

Large amounts of coronal material are propelled outward into interplanetary space by Coronal Mass Ejections (CMEs). Thus one might expect to find evidence for expanding flux ropes in the solar wind as well. To prove this assumption magnetic clouds were analyzed and correlated with H-observations of disappearing filaments. When clouds were found to be directly associated with a disappearing filament, the magnetic structure of the cloud was compared with that of the associated filament. Additionally the expansion of magnetic clouds was examined over a wide range of the heliosphere and compared with the expansion observed for erupting prominences.     

Observational support of reconnection in solar flares

We present a detailed analysis of the magnetic topology of flaring active region. TheH kernels are found to be located at the intersection of the separatrices with the chromosphere when the shear, deduced from the fibrils or/and transverse magnetic field direction, is taken into account. We show that the kernels are magnetically connected by field lines passing close to the separator. We confirm, for other flares, previous studies which show that photospheric current concentrations are located at the borders of flare ribbons. Moreover we found two photospheric current concentrations of opposite sign, linked in the corona by field lines which follow separatrices. These give evidence that magnetic energy is released by reconnection processes in solar flares.     

MHD Spectroscopy of Transonic Flows

In previous publications (Keppens et al.: 2002, Astrophys. J. 569, L121; Goedbloed et al.: 2004a, Phys. Plasmas 11, 28), we have demonstrated that stationary rotation of magnetized plasma about a compact central object permits an enormous number of different MHD instabilities, with the well-known magneto-rotational instability (Velikhov, E. P.: 1959, Soviet Phys.–JETP Lett. 36, 995; Chandrasekhar, S.: 1960, Proc. Natl. Acad. Sci. U.S.A. 46, 253; Balbus, S. A. and Hawley, J. F.: 1991, Astrophys. J. 376, 214) as just one of them. We here concentrate on the new instabilities found that are driven by transonic transitions of the poloidal flow. A particularly promising class of instabilities, from the point of view of MHD turbulence in accretion disks, is the class of trans-slow Alfv’en continuum modes, that occur when the poloidal flow exceeds a critical value of the slow magnetosonic speed. When this happens, virtually every magnetic/flow surface of the disk becomes unstable with respect to highly localized modes of the continuous spectrum. The mode structures rotate, in turn, about the rotating disk. These structures lock and become explosively unstable when the mass of the central object is increased beyond a certain critical value. Their growth rates then become huge, of the order of the Alfv’en transit time. These instabilities appear to have all requisite properties to facilitate accretion flows across magnetic surfaces and jet formation.     

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.      

求解最小费用最大流问题的一种方法

介绍了最大流问题的多解,提出了通过调整圈来求解最小费用最大流的方法。     

Stability and waves of transonic laboratory and space plasmas

The properties of magnetohydrodynamic waves and instabilities of laboratory and space plasmas are determined by the overall magnetic confinement geometry and by the detailed distributions of the density, pressure, magnetic field, and background velocity of the plasma. Consequently, measurement of the spectrum of MHD waves (MHD spectroscopy) gives direct information on the internal state of the plasma, provided a theoretical model is available to solve the forward as well as the inverse spectral problems. This terminology entails a program, viz. to improve the accuracy of our knowledge of plasmas, both in the laboratory and in space. Here, helioseismology (which could be considered as one of the forms of MHD spectroscopy) may serve as a luminous example. The required study of magnetohydrodynamic waves and instabilities of both laboratory and space plasmas has been conducted for many years starting from the assumption of static equilibrium. Recently, there is a outburst of interest for plasma states where this assumption is violated. In fusion research, this interest is due to the importance of neutral beam heating and pumped divertor action for the extraction of heat and exhaust needed in future tokamak reactors. Both result in rotation of the plasma with speeds that do not permit the assumption of static equilibrium anymore. In astrophysics, observations in the full range of electromagnetic radiation has revealed the primary importance of plasma flows in such diverse situations as coronal flux tubes, stellar winds, rotating accretion disks, and jets emitted from radio galaxies. These flows have speeds which substantially influence the background stationary equilibrium state, if such a state exists at all. Consequently, it is important to study both the stationary states of magnetized plasmas with flow and the waves and instabilities they exhibit. We will present new results along these lines, extending from the discovery of gaps in the continuous spectrum and low-frequency Alfvén waves driven by rotation to the nonlinear flow patterns that occur when the background speed traverses the full range from sub-slow to super-fast. This revised version was published online in August 2006 with corrections to the Cover Date.     

圆柱-平板角区湍流流动控制的风洞试验研究

角区流动中马蹄涡系的存在通常会造成不良影响。对圆柱-平板角区流动,在圆柱上游放置一倾斜的小圆棒能够改变角区流动结构。利用油流法和平板表面压力测量方法探讨了湍流流态下不同的小圆棒对平板表面的摩擦力线和压力分布的影响。油流实验揭示了倾斜棒能够改变角区的三维分离,新的分离线由倾斜棒和圆柱共同作用引起;倾斜棒对角区的作用可归类为两种不同的物理现象;倾斜棒能够引起圆柱侧面的分离线向下游发生极大的迁移,导致圆柱底部区域尾迹变窄。平板表面压力测量实验揭示附加的倾斜棒能够极大地改变压力分布情况,角区的逆压梯度相应减小;由此,逆压梯度引起的三维分离必然被削弱。     

Dynamic behavior and topology of 3D magnetic fields

We investigate numerically the dynamical evolution of a boundary driven, topologically complex low plasma. The initial state is a simple, but topologically nontrivial 3D magnetic field, and the evolution is driven by forced motions on two opposite boundaries of the computational domain. A large X-type reconnection event with a supersonic one-sided jet occurs as part of a process that brakes down the large scale topology of the initial field. An energetically steady state is reached, with a double arcade overall topology, in which the driving causes continuous creation of small scale thin current sheets at various locations in the arcade structures.     

MKDVB and CKB Shock Waves

This review presents results from MKDVB and CKB systems to illustrate the properties of magnetohydrodynamics intermediate shock waves. The intermediate shocks can have a family of shock structures; the shock structure and the evolution are related. Furthermore, there exists a class of time-dependent intermediate shocks. This revised version was published online in August 2006 with corrections to the Cover Date.     

Magnetohydrodynamic simulation of a streamer beside a realistic coronal hole

Existing models of coronal streamers establish their credibility and act as the initial state for transients. The models have produced satisfactory streamer simulations, but unsatisfactory coronal hole simulations. This is a consequence of the character of the models and the boundary conditions. The models all have higher densities in the magnetically open regions than occur in coronal holes (Noci,et al., 1993).     

基于Delaunay背景网格插值和局部网格重构的变形体动态混合网格生成技术

建立了一种基于Delaunay背景网格插值方法和局部网格重构方法相结合的变形体动态混合网格生成方法.首先利用作者发展的定态混合网格生成技术生成变形体初始网格,即变形体附近利用结构化的四边形网格,外场采用自适应Cartesian网格,中间由三角形网格过渡.当物体运动或变形时, 首先利用Liu和Qin提出的基于Delaunay背景网格的插值方法对变形体附近的网格进行变形;当物体运动或变形位移很大导致局部网格质量急剧下降、甚至网格相交时,则在局部重新生成网格.利用该方法生成了多种变形体外形的动态混合网格,如单个