磁悬浮径向球面纯电磁磁轴承的设计

针对柱面磁轴承偏转时干扰力矩较大问题,本文提出一种径向球面纯电磁磁轴承设计方法。在本设计中,当磁轴承产生偏转或偏移时,电磁力会指向转子球心,从而降低定子磁极对转子产生的干扰力矩,提高磁轴承的控制精度。首先,阐述球面磁轴承的工作原理并建立数学模型,运用等效磁路理论方法和有限元数值方法分析其电流刚度和位移刚度,2种方法的计算结果基本吻合,表明球面磁轴承的有限元分析模型是合理的。接着,运用有限元方法分析球面磁轴承和柱面磁轴承产生偏转时的干扰力矩,结果表明当转子达到最大偏转角0.3°时,球面磁轴承的干扰力矩是柱面磁轴承的干扰力矩的1.8%,表明球面磁轴承相对于柱面磁轴承在抗干扰力矩能力方面有很大的提高。最后,进一步分析球面磁轴承产生X方向或Z方向偏移时的干扰力矩,计算结果与偏转时干扰力矩的量级相当。综上所述,本文提出的径向球面纯电磁磁轴承有低干扰力矩的优点,可用于航天航空工程中惯性执行机构的高精度控制和角速率检测。     

15-5PH沉淀硬化不锈钢磁粉检测磁痕分析

针对航空15-5PH马氏体沉淀硬化不锈钢在磁粉检测过程中发现的条状、片状和长直磁痕显示进行了总结。分析了不同磁痕显示的特点及微观组织情况,最终确定了磁痕的性质。结合不同热处理状态下的磁特性分析,确立了纯洁度磁粉检测的工艺流程以及磁痕判别方法。研究发现沉淀硬化不锈钢在磁粉检测过程中磁痕显示主要是由铁素体和组织不均匀造成的。研究结论为航空制造过程中沉淀硬化不锈钢的磁粉检测的磁痕判定以及规范的制定提供依据,确保磁粉检测工作的顺利进行。     

航磁补偿技术及补偿质量的评价方法

航磁补偿的目的是要消除飞机平台引入的干扰磁场,对于高精度航空磁探来说,磁补偿质量直接制约了探测效果。文章按照航磁补偿的执行步骤进行了飞机平台磁干扰建模、模型参数求解方法、补偿飞行方案。另外,为了对补偿飞行的质量进行有效控制,采用量化指标对磁补偿效果进行评价,判定补偿效果的优劣。最后,基于 MFC软件平台开发了航磁补偿系数求解及补偿质量评价软件。     

空空导弹惯性开关中圆周磁场对导弹性能的影响

为了提高空空导弹的作战效能和可靠性,由弹载电源向开关电路进行大电流放电,可提高惯性开关中圆柱电极上周磁场的强度,增强抵抗磁钢对钢珠反向作用力的能力,当导弹撞击目标过载较小时,使惯性开关的导通时间也能够满足触发电路工作需要,因此,导弹遇目标不炸的故障概率可得到下降。     

基于磁路法与等效热网络法的航天 永磁同步电机设计与仿真

针对航天永磁同步电机方案初步设计耗时长、过度依赖商业软件的问题,基于磁路法和热网络法,提出了一套方案设计阶段航天永磁同步电机磁热性能快速预估与仿真方法。给出了定子内径、定子外径、铁芯长度、匝数等关键参数的取值准则,建立了包含36个节点集总参数热网络模型,并以端部绕组为例给出了热平衡方程的详细推导过程。通过与成熟商业软件对比,其电磁计算最大误差出现在电流有效值上,偏差值为607%;与样机实测值对比,绕组温升最大误差为73%,满足方案设计阶段预示精度要求,为方案设计阶段航天永磁同步电机快速性能预估提供有力支撑。     

永磁约束电子束轨迹实验研究

通过设计并运用一种直流电子束轨迹简易测量方法,开展了永磁约束电子束轨迹实验研究,得到了永磁铁环对60~80 ke V电子束约束作用的实验数据。结果表明:该测量方法方便有效,结果较为准确;永磁铁对电子束聚焦作用明显,并呈现出一定的规律性。对永磁铁约束电子束研究工作奠定了基础。     

基于马鞍形磁场的永磁直线电机位置解算方法

针对直线电机转子位置检测低成本和较高精度的要求,提出了一种基于马鞍形磁场来获得位置信息的方法及实现过程。分析了永磁体表面的磁场分布特征,指出了利用马鞍形磁场分布曲线来解算位置信息的优点,提出了根据马鞍形磁场推算位置信息的算法流程:先测得错开相位的2条马鞍形曲线数据,划分为4个象限后建立数据库;位置检测时,运用区间搜索算法寻得实际角度所在区间;再根据精度要求,采用合适的插值算法计算得到待解算的角度。仿真结果表明:基于马鞍形磁场的位置解算,能较好地得到直线电机转子的位置信息。     

磁悬浮火箭发动机推力测试台

将电磁悬浮技术用于火箭发动机推力测试试验台是一次新的尝试。本文给出了应用电磁悬浮技术的发动机推力测试试验台的结构,推导了系统的运动方程,并对试验台进行了系统仿真。最后对整个试验台成功进行了多发现场试验,仿真结果和试验结果都表明电磁悬浮技术用于火箭发动机推力测试是成功的,提高了测试系统的性能和推力测试精度。     

Relationship Between Substorm Auroras and Processes in the Near-Earth Magnetotail

Although the auroral substorm has been long regarded as a manifestation of the magnetospheric substorm, a direct relation of active auroras to certain magnetospheric processes is still debatable. To investigate the relationship, we combine the data of the UV imager onboard the Polar satellite with plasma and magnetic field measurements by the Geotail spacecraft. The poleward edge of the auroral bulge, as determined from the images obtained at the LHBL passband, is found to be conjugated with the region where the oppositely directed fast plasma flows observed in the near-Earth plasma sheet during substorms are generated. We conclude that the auroras forming the bulge are due to the near-Earth reconnection process. This implies that the magnetic flux through the auroral bulge is equal to the flux dissipated in the magnetotail during the substorm. Comparison of the magnetic flux through the auroral bulge with the magnetic flux accumulated in the tail lobe during the growth phase shows that these parameters have the comparable values. This is a clear evidence of the loading–unloading scheme of substorm development. It is shown that the area of the auroral bulge developing during substorm is proportional to the total (magnetic plus plasma) pressure decrease in the magnetotail. These findings stress the importance of auroral bulge observations for monitoring of substorm intensity in terms of the magnetic flux and energy dissipation.     

Geoeffectivity of Coronal Mass Ejections

Coronal mass ejections and post-shock streams driven by them are the most efficient drivers of strong magnetospheric activity, magnetic storms. For this reason there is considerable interest in trying to make reliable forecasts for the effects of CMEs as much in advance as possible. To succeed this requires understanding of all aspects related to CMEs, starting from their emergence on the Sun to their propagation to the vicinity of the Earth and to effects within the magnetosphere. In this article we discuss some recent results on the geoeffectivity of different types of CME/shock structures. A particularly intriguing observation is that smoothly rotating magnetic fields within CMEs are most efficient in driving storm activity seen in the inner magnetosphere due to enhanced ring current, whereas the sheath regions between the shock and the ejecta tend to favour high-latitude activity.