磁层亚暴过程中高速流分布

采用实际的磁尾位型,利用数值模拟方法研究磁层亚暴过程中高速流分布。结果表明垂直磁场的高速流主要分布在电流片内,范围在|Z|<0.25RE;平行磁场高速流分布区域在两个区域较大,一个是距离地球较近的磁场较强的区域,另一个是距离等离子体片较近磁场较强的区域。     

硬磁-软磁双层膜中的磁化行为与磁能积

采用蒙特卡罗方法讨论了硬磁-软磁双层膜中的磁化行为与双层膜中磁参量之间的关系.结果表明:硬磁-软磁双层膜中剩余磁化强度随硬磁层或软磁层厚度的增加呈单调性减小或增大,相应的矫顽场随硬磁层或软磁层厚度的增加近似呈单调性增大或减小;而其磁能积的变化是非单调性的,存在磁能积极大值点,该极大值点依赖于硬磁-软磁层的厚度比、各自的饱和磁化强度和单轴各向异性等;硬磁-软磁双层膜的磁化总是从膜边界向膜中间推进,最终带动难轴方向的边界畴转变,且软磁层磁化先于硬磁层,但在软磁层厚度小于临界尺寸的情况下,软磁层与硬磁层的磁化反转趋于同步.     

磁层顶电子剪切流K-H不稳定性

磁层顶是由经过舷激波的太阳风和地磁层相互作用而形成的边界层,其上有电流流动.本文将这种电流看成电子剪切流,来讨论夜侧磁层顶的电子剪切流所引起的Kelvin-Helmholtz(K-H)不稳定性问题.电子剪切流受到的洛仑兹力中包括了电场的作用,正是这种作用使得剪切不稳定性要复杂一些.本文对电子剪切流激发的K-H不稳定性进行了细致的分析,从而得知,电子流剪切引起的K-H不稳定性倾向于在磁层顶内侧激发,并且只有当剪切速率在上下两阈值之间时,才可能激发K-H不稳定性.本文对比了夜侧近地磁层顶和磁尾磁层顶,发现当磁层顶两侧电子数密度之比恒定时,高电子数密度的磁层顶侧易产生K-H不稳定性.而磁鞘侧电子数密度n2与磁层侧电子数密度n1之比n2/n1的改变对不稳定性的影响也很显著:较大的n2/n1产生的K-H波主要是在低速区域,其有效增长率较小.     

场向电流与地磁和亚暴活动的相关性

检验了场向电流与地磁和亚暴活动的相关性。按极光电集流指数AL的大小,地磁活动被分为4个水平,即|AL|<=50,50<|AL|<=150,150<|AL|<=300和|AL|>300分别相应于非常平静、平静、扰动和强烈扰动。统计结果表明,场向电流的发生率、强度和密度都随地磁活动的增加而增大。在最低活动水平,发生率只有8.9%,而73.2%的事件发生在扰动水平以上。对于夜间的场向电流,65.5%的事件伴随着磁层亚暴。     

反铁磁耦合纳米体系磁特性的微磁学研究

采用微磁学方法研究了磁层间反铁磁耦合强度对SyAF纳米体系磁特性的影响.当SyAF纳米体系上、下磁层间的反铁磁耦合强度不同时,SyAF纳米体系具有两种不同类型的磁滞回线.当磁层间反铁磁耦合强度较小时,体系的矫顽力随反铁磁耦合强度的增大而增大,反磁化机制为反磁化核的形成与传播的反转过程.而当磁层间反铁耦合强度较大时(0.2×10-3J.m-2),体系的矫顽力基本不随反铁磁耦合强度变化,并且在剩磁态为稳定的单畴结构,反磁化机制为类一致反转过程.这类SyAF纳米体系更适合于作为磁信息器件中自旋阀的自由层.     

亚暴期间场向电流的特征

分析了由ISEE-1和ISEE-2飞船在亚暴期间观测到的场向电流的特性,包括场向电流所伴随的行星际磁场、地方时与L值分布以及场向电流强度和密度随亚暴位相的变化,并着重分析了亚暴电流楔的特征。结果表明,亚暴膨胀相的场向电流强度和密度都达到极大值;亚暴的膨胀相是由行星际磁场转向或南向分量变小触发的,其起始位置很可能位于近地等离子体片内边缘。     

大型发电机失磁过程及失磁保护动作特性分析

在电力系统保护中,同步发电机的失磁保护是最重要的保护之一.励磁故障涉及发电机大干扰稳定性,是一个复杂并难以解决的问题.大型发电机失磁过程伴随着定子侧电压,电流、有功、无功,转子侧励磁电压、电流以及转差的交错变化;对失磁过程中电磁量的变化进行详细分析是改进和完善发电机失磁保护的基础.现有的保护判据在非失磁的其他工况下均有可能误动,因此,对不同失磁保护的动作特性进行研究就十分有必要.通过Matlab分析失磁过程中电气量的变化,对现有几种保护判据的动作特性进行分析.     

关于磁重联区三维磁零点的卫星观测研究

磁重联是等离子体中磁场能量快速转换为粒子动能和热能的主要途径,是空间物理和等离子体物理中的重要现象.磁重联过程发生在磁场的拓扑分形面上;这种分形面一般是由磁零点附近磁场梯度张量的本征矢量确定的.磁零点的三维特性要求至少空间4点的同时测量.Cluster计划提供了迄今为止唯一的卫星测量手段.基于Poincare指数方法分析Cluster卫星在地球磁尾的探测数据,(1) 找到了磁重联过程中存在4种磁零点的证据;(2) 发现磁零点周围磁场的空间特征尺度大约为离子惯性长度,从而首次揭示霍尔效应可能在三维磁重联中起重要作用;(3) 在重联区找到匹配的磁零点对,并计算出零点连线的长度,确定了所产生的磁场的拓扑分形面;(4) 发现在零点连线附近存在低杂波频率的电磁振荡,这为磁重联过程中可能的电子加速、加热机制提供了观测基础.     

溅射工艺对NiFe/Cu复合丝结构和性能的影响

利用射频磁控溅射法分别采用连续溅射和间歇溅射工艺制备了Ni80Fe20/Cu复合结构丝。通过扫描电镜和X射线衍射等手段研究了溅射模式对复合丝微观结构的影响.结果表明：间歇溅射使镀层之间形成明显的界面,镀层结晶度增加,晶粒较大.利用巨磁阻抗效应和磁滞回线手段分析了样品的磁性能,发现实验中溅射的磁性层具有良好的软磁性能,复合丝呈现出较大的巨磁阻抗效应.当采用间歇溅射工艺时,由于复合丝的镀层中存在明显界面,内、外磁层的磁化行为不同,出现两个各向异性场.该样品经退火后,释放了一部分内部应力,软磁性能提高,阻抗效应增强,且内、外磁层磁性能趋于一致.     

基于空间矢量理论异步电动机起动过程的控制

为了提高异步电动机的起动性能,对异步电动机的起动过程进行了研究.在空间矢量理论的基础上,导出以定子电流矢量、转子磁链矢量为核心变量的动态方程.通过仿真分析和动态方程理论分析,揭示了异步电动机在非受控状态下全压起动时转子转速、电磁转矩、定子电流、转子磁链的变化过程,指出异步电动机起动时起动电流大而起动转矩并不大的主要原因在于起动时磁场建立过程的不平稳性.以此为基础,提出采用预励磁及全过程控制定子电流矢量转速和幅值的方法,使转子磁链矢量平稳建立且与定子电流矢量同步旋转.最后仿真和实验结果表明该方法可在大大减小起动电流幅值的情况下达到全压起动同样的效果,起动性能明显提高.     

Correlation between continuous lobe reconnection in the mid magnetotail and substorm expansion onset

Data on plasma sheet crossing measured by Cluster/HIA and Cluster/FGM during the period from July to October in 2001 -2003 are analyzed. Based on previous work on the characteristic features of continuous lobe reconnection (CLR) described in reference, two case studies and a statistical analysis were carried out on correlation between CLR in the mid magnetotail and substorm expansion onset for the events occurring during this period. It is found that almost all CLR events are in close connection with substorms. The beginning of CLR is almost always a few minutes ahead of substorm activities seen in the near Earth magnetotail and on the ground-based stations. This provides a clear indication that CLR is the virtual cause of substorm expansion onset during the period of continuous southward interplanetary magnetic field.     

Auroral substorm response to solar wind pressure shock

Two cases of auroral substorms have been studied with the Polar UVI data, which were associated with solar wind pressure shock arriving at the Earth. The global aurora activities started about 1–2 min after pressure shocks arrived at dayside magnetopause, then nightside auroras intensified rapidly 3–4 min later, with auroral substorm onset. The observations in synchronous orbit indicated that the compressing effects on magnetosphere were observed in their corresponding sites about 2 min after the pressure shocks impulse magnetopause. We propose that the auroral intensification and substorm onset possibly result from hydromagnetic wave produced by the pressure shock. The fast-mode wave propagates across the magnetotail lobes with higher local Alfven velocity, magnetotail was compressed rapidly and strong lobe field and cross-tail current were built in about 1–2 min, and furthermore the substorm was triggered due to an instability in current sheet.     

Nonlinear dependence of anomalous resistivity on the reconnecting electric field in the Earth’s magnetotail

Based upon the observational data of the fast magnetic reconnection in the nearly collisionless magnetotail and the particle in cell (PIC)simulations on the electron acceleration in the reconnecting current sheet with guide magnetic field,we self consistently solved one dimension Vlasov equation with the magnetotail parameters and realistic mass ratio to explore the relationship between the anomalous resistivity and the induced electric field.As compared with theoretic formula for the current driven ion-acoustic and Buneman anomalous resistivity,the anomalous resistivity may result from the ion acoustic instability for small reconnecting electric field and the Buneman instability for large reconnecting electric field.The discrepancy between the theoretic results and numerical simulations may be caused by the high frequency instability that results from the deviation of electron distribution from Maxwellian one.These results are consistent with the early experimental results and favorable for the fast reconnection to take place.     

Observations of kinetic Alfvén waves by THEMIS near a substorm onset

Low frequency electromagnetic fluctuations in the vicinity of a magnetospheric substorm onset were investigated using simultaneous observations by THEMIS multiple probes in the near-Earth plasma sheet in the magnetotail.The observations indicate that in the vicinity of a substorm onset,kinetic Alfvén waves can be excited in the high-βplasma sheet(β=2μ0nT/B 2 ,the ratio of plasma thermal pressure to magnetic pressure)within the near-Earth magnetotail.The kinetic Alfvén wave has a small spatial scale in the high-βplasma.The parallel electric field accompanying kinetic Alfvén waves accelerates the charged particles along the magnetic field.The kinetic Alfvén waves play an important role in the substorm trigger process,and possibly in the formation of a substorm current wedge.     

A preliminary exploration of the mechanism for the occurrence of two types of various magnetic structures in the magnetotail

As well known, the magnetic cross-tail component B_y in the magnetotail is in direct proportion to the in-terplanetary magnetic field (IMF) B_y component. And the polarity of IMF and plasmoid / flux rope B_y components do indeed agree. This results indicate that the IMF B_y penetrates plasmoids and the magnetic structures must therefore be three-dimensional. In this note, the dynamical processes of magnetotail in the course of a substorm are studied using a MHD code with two-dimensions and three components on the basis of two types of initial equilibrium solutions of the quiet magnetotail. The numerical results of two cases illustrate various features of time evolution of B_y component that correspond to two kinds of plasmoid-like structures: one is associated with a flux rope core and the other resembles a “closed loop” plamoid. Therefore, the occurrence of various magnetic structures in the magnetotail might be related to nonsteady driven reconnection with different distributions of the B_y component.     

THEMIS observation of a magnetotail current sheet flapping wave

A flapping wave was observed by THEMIS-B （P1） and THEMIS-C （P2） probes on the dawn side of the magnetotail, while the solar wind was generally stable. The magnetic activity was quite weak, suggesting that this flapping wave was generated by an internal instability, which normally occurs during magnetic quiet times. Our analysis shows that the flapping wave was propagating downward with a tail-aligned scale of at least 3.7 RE and did not show much change in shape during its propagation from P1 to P2. Correlation analysis employed to estimate the time lag between the corresponding half waveforms of P1 and P2 shows that the propagating velocities along the current sheet normal directions were close to each other in the beginning, but increased linearly later on. The average wavelength of the flapping wave is approximately 4 RE. Theoretical analysis suggests that the ballooning type wave model may not be the mechanism for the observed flapping wave, but that the magnetic double-gradient instability model is a more plausible candidate.     

Continuous lobe reconnection in the mid-tail and its relationship to substorms： Cluster observations of continuous lobe reconnection in the mid-magneto tail

When the IMF turns southward, a great amount of magnetic energy is stored in the magnetotail, and the electric field across the magnetotail substantially enhances. As long as magnetic reconnection （MR） in the magnetotail initiates and continues, the magnetic field and plasma in the central plasma sheet are carried away to the near-Earth and down to the tail, the magnetic field and plasma in the lobe region enter the CPS and are involved in MR. We call this process “Continuous Lobe Reconnection （CLR）”. In this paper a detailed analysis of Cluster observation of MR through 2001--2003 is made. Plenty of CLR events are found that led to considerable changes of tail configuration, appearance of BBF, as well as large-scale bubbles in which both plasma temperature and number density substantially decrease. It is shown that in general CLR events last for dozens of minutes and have good correspondence to substorm initiation under the condition of continuous southward IMF.     

Downward current electron beams observed at the dipolarization front

The strong field-aligned pitch angle distribution of electrons is observed right at the dipolarization front (DF) before the arriving of a high speed flow when the four Cluster satellites are traveling in the magnetotail around 15 R E on July 22, 2001. The increased electron fluxes only last for a short time period at the DF, corresponding to just a few bouncing periods for 1 keV electrons. The field-aligned current contributed by these electrons agrees well with that calculated by the magnetic field observations by four satellites at the front. These electron streams are found in the energy range of 0.2-2 keV, peak around 1 keV. It is suggested that these downward current electrons may be originated near the aurora region by some kinds of potential structure. The occurrence of these electrons implies that the formation of the dipolarization front and the associated field-aligned current play an important role in the magnetosphere-ionosphere coupling.     

In situ detection of collisionless reconnection in the Earth's magnetotail

Magnetic reconnection is the process by which magnetic field lines of opposite polarity reconfigure to a lower-energy state, with the release of magnetic energy to the surroundings. Reconnection at the Earth's dayside magnetopause and in the magnetotail allows the solar wind into the magnetosphere. It begins in a small 'diffusion region', where a kink in the newly reconnected lines produces jets of plasma away from the region. Although plasma jets from reconnection have previously been reported, the physical processes that underlie jet formation have remained poorly understood because of the scarcity of in situ observations of the minuscule diffusion region. Theoretically, both resistive and collisionless processes can initiate reconnection, but which process dominates in the magnetosphere is still debated. Here we report the serendipitous encounter of the Wind spacecraft with an active reconnection diffusion region, in which are detected key processes predicted by models of collisionless reconnection. The data therefore demonstrate that collisionless reconnection occurs in the magnetotail.