Response of the Earth＇s Magnetosphere and Ionosphere to Solar Wind Driver and Ionosphere Load： Results of Global MHD Simulations

Three-dimensional global magnetohydrodynamic simulations of the solar wind-magnetosphere-ionosphere system are carried out to explore the dependence of the magnetospheric reconnection voltage, the ionospheric transpolar potential, and the field aligned currents （FACs） on the solar wind driver and ionosphere load for the cases with pure southward interplanetary magnetic field （IMF）. It is shown that the reconnection voltage and the transpolar potential increase monotonically with decreasing Pedersen conductance （∑ p ）, increasing southward IMF strength （Bs） and solar wind speed （Vsw）. Moreover, both regions 1 and 2 FACs increase when Bs and vsw increase, whereas the two currents behave differently in response to ∑p. As ∑p increases, the region 1 FAC increases monotonically, but region 2 FAC shows a non-monotonic response to the increase of ∑p ： it first increases in the range of （0,5） Siemens and then decreases for ∑p 〉 5 Siemens.     

Earth＇s Magnetosphere Impinged by Interplanetary Shocks of Different Orientations

Using a recently developed PPMLR-MHD code, we carry out a global numerical simulation of the interaction between interplanetary shocks and Earth＇s magnetosphere. The initial magnetosphere is in a quasi-steady state, embedded in a uniform solar wind and a spiral interplanetary magnetic field （IMF）. An interplanetary （IP） shock interacts in turn with the bow shock, the magnetosheath, the magnetopause, and the magnetosphere, and changes the magnetosphere in shape and structure, and the distribution of the electric current and potential in the ionosphere as well. A preliminary comparison is made between two IP shocks of the same solar wind dynamic pressure and a vanishing IMF Bz on the downstream side, but with different propagation directions, one parallel and the other oblique to the Sun-Earth line. The numerical results show that both shocks cause a compression of the magnetosphere, an enhancement of magnetic field strength and field-aligned current in the magnetosphere, and an increase of the dawn-dusk electric potential drops across the polar ionosphere. Moreover, the magnetosphereionosphere system approaches a similar quasi-steady state after the interaction, for the downstream states are very close for the two shocks. However, the evolution processes of the system are remarkably different during the interaction with the two shocks of different orientations. The shock with the normal oblique to the Sun-Earth line results in a much longer evolution time for the system. This demonstrates that the shock orientation plays an important role in determining the associated geophysical effects and interpreting multisatellite observations of IP shock-magnetosphere interaction events.     

Observational Aspects of Magnetic Reconnection at the Earth’s Magnetosphere

Magnetic field reconnection has shown to be the dominant process in the solar wind-Earth’s magnetosphere interaction. It enables mass, momentum, and energy exchange between different plasma regimes, and it is regarded as an efficient plasma acceleration and heating mechanism. Reconnection has been observed to occur in laboratory plasmas, at planetary magnetospheres in our Solar System, and the Sun. In this work, we focus on analyzing the characteristics of magnetic reconnection at the Earth’s magnetosphere according to spaceborne observations in the vicinity of our planet. Firstly, the locations where magnetic field reconnection are expected to occur within the vast magnetospheric region are addressed, and is shown how they are influenced by changes in the interplanetary magnetic field direction. The main magnetic field and plasma signatures of magnetic reconnection are discussed from both theoretical and observational points of view. Spacecraft observations of ion inertial length scale reconnection are also presented.     

Analytic Description of High Poloidal Beta Equilibrium with a Natural Inboard Poloidal Field Null

Analytical solutions of the Grad-Shafranov equation are always useful because of their convenience and accuracy in theoretical study of stability, transport and kinetic analysis. For the quasi-uniform toroidal current density case, the so-called Solov＇ev configuration is the earliest one that was widely used for the magnetohydrodynamic （MHD） stability analysis and also used as benchmark for equilibrium code studies later.     

基于MHD的磁射流抛光中流场的分析与模拟

从理论上分析了磁射流抛光中的磁场与流场的相互作用,构建了磁射流抛光的冲击射流模型,基于磁流体动力学对磁射流抛光过程的紊动冲击射流进行数值模拟,得到了磁射流抛光过程的连续流场和射流在工件壁面上的压力、速度、紊动强度分布。通过比较射流抛光和磁射流抛光的数值计算结果,分析了磁流变效应对射流稳定性的影响,从射流的流场、速度、紊动强度等方面分析射流在磁场中稳定的原因。     

Magnetic Behaviour of Tb/Si Nanoscale Multilayers with Small Thickness of Rare Earth Layers

We report the magnetic properties of Tb/Si multilayers obtained by rf-sputtering at the Tb layer thickness LTb = 3 nm. Analysis of the magnetization processes indicates more complex behaviour than canonical spinglass transition. It is more probable that these multilayers contain both Tb superparamagnetic particles and Tb-Si spin-glass alloys.     

ULF Waves Associated with Solar Wind Deceleration in the Earth＇s Foreshock

Characteristics of ULF waves associated with the solar wind deceleration in the Earth＇s foreshock on 6-7 April 2003 is studied using the wave telescope technique. In the satellite frame, the ULF waves are the left-handed polarized and quasi anti-parallel propagating mode, with a power peak at about 18.63mHz. The wave vector in the GSE coordinates is estimated to be k = （-4.29, 2.28, 1.21）×10^-4 km^-1, In the solar wind frame, the frequency of waves becomes - 9.39 mHz after the Doppler shift correction. The propagation direction of the waves is thus reversed and correspondingly the polarization of the waves becomes right-handed. The above-mentioned characteristics of the ULF waves in the solar wind frame indicate that the ULF waves associated with the solar wind deceleration are the Alfven-whistler waves, which have been frequently reported in both the observations and computer simulations.     

Shock Compression and Phase Transitions of Magnesiowiistite （Mg,Fe）O up to Earth＇s Lowermost Mantle Conditions

We report new shock-compression data for polycrystalline （Mg,Fe）O up to 130 GPa shock pressures corresponding to Earth＇s lowermost mantle conditions. Our data together with the existing shock-wave data of （Mg, Fe）O and its end-members MgO and FeO reveal that the Hugoniot curves of （Mg,Fe）O does not change with varying FeO content for their B1 phase （NaCl-structure） in the pressure-relative-volume plane. The evidence of the volume change within 3% at around 120GPa along the Hugoniot of （Mgo.6, Feo.4）O is consistent with a structural transition from B1 phase （NaC1 cubic） to B8 phase （NiAs-type hexagonal）. Such a structural transition of （Mg, Fe）O, if indeed occurs, may in part contribute to the scattering of seismic waves and change in velocity gradient found in the lowermost mantle.     

能量输运对柱状等离子体开关磁场穿透过程的影响

 对于高密度、导通时间为μs级的柱状等离子体开关,利用磁流体动力学理论(MHD),对其导通阶段的磁场穿透过程进行了模拟,得到了磁场分布随时间的变化;研究了开关导通过程中能量输运导致的温度不均匀分布对磁场穿透过程的影响。模拟结果表明：对于高密度等离子体开关,磁场以远大于磁扩散速率的速度穿透到等离子体中;在磁压对等离子体产生的压缩效应和欧姆加热效应共同作用下,激波区域的等离子体温度显著升高,这进一步加速了磁场穿透;当考虑能量输运方程时,开关导通时间为0.87 μs,比等温模型的结果0.92 μs短,与实验结果0.87 μs相一致。     

能量输运对柱状等离子体开关磁场穿透过程的影响

对于高密度、导通时间为μs级的柱状等离子体开关,利用磁流体动力学理论(MHD),对其导通阶段的磁场穿透过程进行了模拟,得到了磁场分布随时间的变化;研究了开关导通过程中能量输运导致的温度不均匀分布对磁场穿透过程的影响。模拟结果表明：对于高密度等离子体开关,磁场以远大于磁扩散速率的速度穿透到等离子体中;在磁压对等离子体产生的压缩效应和欧姆加热效应共同作用下,激波区域的等离子体温度显著升高,这进一步加速了磁场穿透;当考虑能量输运方程时,开关导通时间为0.87 μs,比等温模型的结果0.92 μs短,与实验结果0.87 μs相一致。     

On the Influence of Propagation Properties of Whistler-Mode Waves in the Earth’s Magnetosphere on Their Cyclotron Amplification

Radiophysics and Quantum Electronics - We study the properties of the cyclotron amplification of whistler-mode waves during their propagation in the Earth’s magnetosphere in the presence of...     

Formation of Singularities in One—Dimensional Hydromagnetic Flow

Two results on the formation of singularities in solutions to the system of one-dimensional hydromagnetic dynamics are presented.In particular,it is shown that shocks form from a smooth spatial periodic flow in a finite time if the initial amounts of entropy and the “magnetic field” in each period are smaller than those of sound waves.A quantitative estimate of blow-up time is also given.     

Two New Solutions of Non-constant-α Force-Free Magnetic Field

Two new solutions for non-constant-α force-free magnetic field are found analytically. Implications of the results to astrophysical solar plasmas as well tokamak plasmas are discussed.     

磁流体加速和磁流体加速风洞

高超声速飞行器对于更高飞行速度的追求，给地面风洞设备模拟能力提出了新的要求，磁流体加速成为一个重要突破方向.文章介绍了国内外在磁流体加速基本原理以及磁流体加速技术应用于地面风洞试验方面的研究工作.基于磁流体（magneto-hydro-dynanic，MHD）加速的高超声速风洞设备可以模拟高超声速飞行器的试验条件，复现超高速的飞行环境，是突破超高速飞行器再入研究地面试验模拟能力的关键技术，在航空航天领域具有重要的研究意义和应用前景.      

涂层裂纹的MHD压降研究

目前的研究已表明,自冷包层中的MHD压降问题可以在与液态金属流体接触的通道壁上涂电绝缘陶瓷涂层或自修复涂层而得到很好的解决。但因热应力等因素引起陶瓷出现裂纹或剥落,在陶瓷涂层出现裂纹或剥落后的MHD压降需要开展相应的实验工作。考虑到低成本和方便的涂层工艺,本研究中的绝缘涂层使用了在回路的运行温度下与流体介质相容的聚氨基甲酸脂,用旋转加热法在外径为64mm、内径为57mm的导电实验段的内壁均匀地涂上2.65mm厚的聚氨基甲酯酯电绝缘涂层,涂后的流道内径为51．7mm,如图1所示,D1－D5为设置的模拟涂层裂纹的铜电极,电要直径为10mm,长为100mm。P1和P2为差压传感器接口,间距为500mm。LEVI探针可测量该方向上的MHD流速分布。P1和P2,电极D1－D5以及LEVI接口均位于电磁铁提供的均匀磁场区域,其方向与液态金属流速和外加磁场垂直。采用特殊的涂层工艺,使每个接口连接处的液态金属不会通过这些电极、差压接口以及LEVI接口与导电的实验段外壁短路,确保全绝缘和各种模拟裂纹的MHD压降实验的可靠性和准确性。     

Propagation of Fast Magnetoacoustic Waves in Stratified Solar Atmosphere

The characteristics of magnetohydrodynamic fast wave propagation in the solar stratified atmosphere are studied by the ray tracing method. The propagation behaviour of the wavefronts is described in detail. A magnetic field incorporating the characteristics field spreading expected in flux tubes is used, which represents the main feature of an active region. Partly ionization is considered beside the stratified solar atmosphere consisting chromosphere, transition region and corona. The study may explain the characteristics in observations of Moreton and extraultraviolet image telescope （EIT） waves. The wavefront incurred by the disturbance initialized at the base of the transition region propagates fast initially due to strong magnetic field, and it slows down when arriving beyond the region of flux-tube. Meanwhile, the wave propagates in the corona with a more consistent speed, as seen in the observation of EIT waves. The speeds and propagated characteristics in chromosphere and corona of the wavefronts are in agreement with those observed in H~ Moreton and EIT waves, respectively.