ICME期间磁暴的太阳风参数和极光沉降能量

基于1995-2004年ICME驱动的强烈磁暴(SA型)、强磁暴(SB型)和延迟型主相暴(SC型)三种磁暴类型,对1AU处太阳风动压、太阳风速度、行星际磁场、EK-L电场以及极光沉降能量进行时序叠加分析,并分别与-vBz耦合函数和Newell耦合函数进行对比.结果表明,三种磁暴在ICME到达前期的太阳风动压较稳定,背景太阳风、极光沉降能量、行星际磁场和磁层存在相对平静期. ICME到达前期SA型磁暴的背景太阳风速度、行星际磁场南向分量以及极光沉降能量的均值高于另外两种磁暴类型,这说明大型日冕物质抛射在ICME到达前就对行星际磁场、背景太阳风和HP产生了影响.磁暴急始后,SC型磁暴的EK-L电场斜率小,峰值延后且行星际磁场北向分量增强,这些都是磁暴主相延迟的表现,极光沉降能量随着行星际磁场转为南向而增加.     

基于Labview的磁罗盘测试系统设计与实现

磁罗盘是无人机航向测量的常用关键部件,为了测试其性能的好坏,设计了一套基于PXI总线计算机等硬件和Labview软件的磁罗盘智能测试系统。该系统能够有效地完成LP-1磁罗盘各项性能测试,具备友好的人机交互界面,能够对测试数据进行保存。实际应用表明,该系统工作稳定、操作简便,在无人机部件装机放飞前能够及时发现磁罗盘部件故障隐患,提高了无人机飞行安全。     

有/无铁芯轴向磁通风力发电机性能研究

针对有、无铁芯轴向磁通风力发电机哪种更适合在微风地区使用,对比分析了有铁芯和无铁芯发电机在不同转速时的效率、转矩特性及电能质量。通过对发电机基本参数的确定,建立有、无铁芯发电机3D有限元模型,对比有、无铁芯风力发电机的运行特性,并通过实验平台验证3D有限元计算结果。研究结果表明：发电机在额定运行状态下,磁钢用量相同时,有铁芯发电机效率比无铁芯发电机效率高4.2%,但有铁芯发电机存在齿槽转矩,发电机运行平稳性差;在磁钢用量及电枢绕组匝数相同时,无铁芯发电机效率比有铁芯发电机效率高0.3%且启动力矩更小;当磁通量相同时,无铁芯发电机效率比有铁芯发电机效率高5.7%,综上所述无铁芯发电机更适合在微风低速下运行。     

航天器内部磁场环境主动补偿方法

为解决空间引力波探测任务中航天器磁场对惯性传感器干扰的问题,研究在航天器复杂磁环境下利用主动测控方式获取小尺度均匀磁场环境的方法.在惯性传感器周围进行分布式磁场探测,并采用球谐函数法或多磁偶极子法实现对惯性传感器外部磁源的估计,计算惯性传感器所处位置的空间磁场及其梯度分布.利用线圈技术,对磁场及其梯度进行线性补偿.讨论分析传感器数量以及磁源布局方式等因素对最终补偿效果的影响.仿真试验结果表明,通过这一方法可将惯性传感器所在区域的磁场及其梯度降低1～2个数量级,降低引力波航天器平台的剩磁控制压力,为引力波探测提供满足要求的磁场环境.      

铝盐絮凝剂复配含磁絮体形成的最佳参数及性能研究

本文系统研究了铝盐及有机高分子絮凝剂与磁粉在高浊度原水中复合投加的絮凝效果和含磁絮体形成的最佳参数,并通过比较处理效果,出水沉降时间和含磁絮体的显微结构,验证了本絮凝方法处理高浊度原水效果更好,停留时间更短的预估,且絮体含磁易分离,为管式絮凝器采用磁絮凝和高梯度磁分离工艺提供了参数依据和高效絮凝分离一体化、管道化的可行性证明。     

Topology of the high latitude magnetosphere during large magnetic storms and the main mechanisms of relativistic electron acceleration

One of the main endeavors of the “Space Weather” program is the prediction of the appearance of very large fluxes of relativistic electrons with energies larger than 1 MeV, because they represent a serious potential hazard for satellite missions. Large fluxes of relativistic electrons are formed in the outer radiation belt during the recovery phase of some storms. The formation of large fluxes is connected to a balance between the acceleration and loss processes. A two-step acceleration process is ordinarily analyzed. A “Seed” population with energies ∼hundreds of keV appeared during expansion phase of magnetospheric substorm. A “Seed” population is additionally accelerated obtaining relativistic energies by some other process. Several acceleration mechanisms have been proposed for the explanation of the electron acceleration, including radial diffusion and internal acceleration by wave-particle interactions. Nevertheless, none of them takes into account great changes of magnetospheric topology during a magnetic storm. Such changes are mainly connected with asymmetric and symmetric ring current development. We analyze the changes of magnetospheric topology during magnetic storms. We show that a change of the magnetospheric magnetic field can be the important factor determining the acceleration of relativistic electrons.     

磁悬浮飞轮技术及其应用研究

针对目前卫星上使用的滚珠轴承动量飞轮的不足,概要介绍了磁悬浮飞轮的优点及其分类。首先综述了应用于卫星姿态控制执行机构的磁悬浮飞轮的发展历史与研究现状,重点分析了磁悬浮飞轮的主要关键技术。其次阐述了两轴主动控制型磁悬浮飞轮应用于卫星姿态控制的适应性,较为全面的介绍了我们在磁悬浮飞轮技术研究上的工作与进展。最后展望了磁悬浮飞轮技术未来应用的发展方向,针对我国空间技术发展的实际需求提出了目前应重点研究的方向。     

一种组合磁钢叠加磁场洛伦兹力磁轴承设计方法

针对现有洛伦兹力磁轴承功耗较高、工作气隙磁场非均匀性问题,提出一种基于组合磁钢叠加磁场的新型洛伦兹力磁轴承设计方法。首先建立了传统洛伦兹力磁轴承电磁力矩模型,揭示了洛伦兹力磁轴承功耗和控制精度与其磁场性能之间的对应关系。在此基础上,引入了磁场强度均值和磁场均匀度的概念,并以此为依据设计出一种轴向整环充磁磁钢与径向分块充磁磁钢组合工作的新型方案。其中轴向充磁磁钢产生主磁场,保证工作气隙周向均匀性,辅助以径向充磁磁钢,使磁场主要聚集在工作气隙处。相比现有洛伦兹力磁轴承,在相同尺寸约束条件下,新型洛伦兹力磁轴承径向磁场均匀度提升了8.7%,磁场强度提升了51.8%,周向磁场连续性显著提高。仿真结果表明,新型洛伦兹力磁轴承可以有效降低功耗、提升控制精度,研究成果可为研制超高精度磁悬浮惯性机构提供一条新的技术途径。     

一种应用于低频电磁波通信的快响应原子磁强计

相较于传统线圈,原子磁强计作为低频电磁波通信信号磁传感接收器具有体积小、灵敏度高的优势。基于射频-光双共振原理实现原子的宏观极化和相干进动,并通过探测磁矩横向分量来获得待测磁场信息,最终实现一台灵敏度500 fT/Hz^1/2@1～5 Hz,响应带宽3.5 kHz的原子磁强计。并利用该原子磁强计作为磁传感器对频率200 Hz、磁场分量幅度10 nT的电磁波开展了通过探测磁场分量接收通信信号的实验,实现码率200/s的电磁波通信信号的接收,验证了该磁强计作为接收机接收低频电磁波通信信号的能力。     

Transient Effects and Disturbed Conditions

In the present phase of the solar cycle no big transients leading to strong modulation had been observed after 1991. Apart from a few minor disturbances cosmic rays were still recovering to a new intensity maximum. It was suggested, therefore, that existing literature from previous cycles should be critically reviewed. The scene was set by the introductory papers on— phenomenology of cosmic ray modulation in successive solar cycles throughout the heliosphere— the present state of models for long term modulation and their shortcomings— the relation between cosmic ray variations and the magnitude of the interplanetary magnetic field (the CR-B-relation)— charge dependent effects.In the discussions, the study of propagating diffusive disturbances and the CR-B-relation played a central role. The difference was stressed between isolated transient disturbances in the inner solar system (Forbush decreases), and the long lasting, step-like decreases caused by merged interaction regions in the outer heliosphere. The recovery rates following the step-like decreases vary with the phase in the 22-year solar cycle. In some cases this requires a modification of existing drift models. In the outer heliosphere, the CR-B-relation leads to the result 1/ between the diffusion coefficient and the field magnitude . This simple result is a challenge for theoreticians to derive the perpendicular diffusion coefficient fromfirst principles. The three articles in this report essentially follow the list of open points and arguments just presented.The article "Observations and Simple Models" is organised around the model of a propagating diffusive barrier, its application to Forbush effects in the inner heliosphere and to decreases caused by merged interaction regions in the outer heliosphere. Acomparison of observed Forbush decreases with model predictions requires a careful separation of the two steps related to the turbulent region behind the shock front and the closed magnetic field regions of the ejecta (the interplanetary counterparts of coronal mass ejections). It is shown that models for propagating disturbances can be used to derive values of the diffusion coefficients phenomenologically, not only during the disturbance, but also in the ambient medium.The "Modeling of Merged Interaction Regions" summarizes the dynamic and time-dependent process of cosmic ray modulation in the heliosphere. Numerical models with only a time-dependent neutral sheet prove to be successful when moderate to low solar activity occurs but fail to describe large and discrete steps in modulated cosmic rays when solar activity is high. To explain this feature of heliospheric modulation, the concept of global merged interaction regions is required. The com-bination of gradient, curvature and neutral sheet drifts with these global merged interaction regions has so far been the most successful approach in explaining the 11-year and 22-year cycles in the long-term modulation of cosmic rays.The "Remarks on the Diffusion Tensor in the Heliosphere" describe available theories of perpen-dicular diffusion and drift, and discuss their relevance to cosmic rays in the heliosphere. In addition, the information about diffusion coefficients and spatial gradients obtained from the analysis of steady state anisotropies at neutron monitor energies is summarized. These topics are intimately related to the other two articles. They are also part of the general discussion about the "Diffusion Tensor throughout the Heliosphere" which played an important role in all working groups.