大尺度场向电流的控制因素

将ＩＳＥＥ－１和ＩＳＥＥ－２飞般测量的地球内磁层场向电流作为行星际磁场与极区地磁活动水平（由ＡＬ表征）的函数。发现大约７５％的场向电流发生在行星际磁场南向时,其余２５％发生在行星际磁场由南向转到北向的半小时内。而且,发生在ＡＬ〈－１５０ｎＴ的场向电流也大约是７５％。场向电流的强度和密度随行星际磁场南向分量及ＡＬ的负值增加而增大。由此而得出结论,内磁层场向电流的产生主要是由行星际磁场控制的,是太阳风     

基于等效磁路法的轴向磁场磁通切换型永磁电机静态特性分析

轴向磁场磁通切换型永磁(AFFSPM)电机是一种轴向长度短、转矩密度高的新型永磁电机。该电机磁场呈三维分布,与径向磁场电机不同,需要对该电机进行三维有限元分析,从而增加了电机分析和优化时的计算时间和成本。基于等效磁路法分析了AFFSPM电机的静态特性,建立了AFFSPM电机的非线性等效磁路模型,采用该模型计算、分析了气隙磁密、空载永磁磁链、反电动势和电感等特性,并与采用三维有限元方法的计算结果进行比较,验证了AFFSPM电机等效磁路模型的准确性,表明等效磁路模型适用于AFFSPM电机初始设计和分析。     

同步磁阻电机定子电流最优控制

针对磁路饱和对同步磁阻电机运行特性的影响,提出了定子电流最优控制策略。通过有限元法对电感与电流的非线性关系进行拟合,并利用拟合结果得到最优定子电流随转矩变化的运行轨迹,以实现同步磁阻电机最大转矩电流比(MTPA)控制;同时对于交直轴电流环相互耦合的问题,提出磁路饱和补偿的电流环设计,以提高其动静态性能。仿真与试验结果验证了该方案的有效性。     

铯光泵原子磁强计研制进展

铯光泵原子磁强计利用极化铯原子自旋拉莫尔相干进动探测和测量磁场,具有精度高、响应快等特点。围绕铯光泵原子磁强计的技术特点,重点介绍了其工作原理及研制工作,实现了一款铯光泵原子磁强计整机。测试结果表明,该款磁强计磁场测量范围为20000~100000nT,峰-峰噪声值为0.0017nT,能满足磁异常探测对高精度磁强计的需求。     

航空磁探中水下目标三维积分方程磁场建模

为获取航空磁探中水下铁磁性目标的空间磁场分布,通过三维积分方程法的基本原理推导出空间磁场的解析式,根据矢量恒等式和高斯散度定理简化空间磁场计算式,建立水下铁磁性目标空间磁场预测模型。通过铁磁性长方体对模型进行理论验证,使用铯光泵磁力仪测量铁磁性长旋转椭球体的高空磁场;然后,基于预测模型推算铁磁性长旋转椭球体的磁场,根据实际测量的磁场数据和预测值进行比较。结果表明,预测模型的推算精度较高,平均绝对误差为0.320 5 nT,平均相对误差为12.368%。     

利用BP神经网络预测AE指数

采用的预报模式是一种全连接的BP网络模型,利用太阳风及行星际磁场的观测数据预报AE指数.神经网络输入选用ACE卫星数据,取5 min平均值,通过比较,选用4个预报参量.构造了预报参量时续为20 min,40 min和60 min依次递增的三个网络,分别进行训练和预测,并对行星际参量对AE指数影响的时续性进行了探讨.预报结果表明,全连接BP神经网络在AE指数的短期预报中是比较有效的,同时还提出了需要进一步改进的环节.      

金属磁记忆微观机理试验研究

金属磁记忆检测机理中指出:地磁场环境中受载荷作用的铁磁试件,其内部会发生具有磁致伸缩性质的磁畴组织定向和不可逆的重新取向。将未经磁化且弯曲不同角度的无取向硅钢片和未经磁化且施加不同载荷的20#钢压缩试件制作成金相观察试样,利用B itter粉纹法观察受力程度不同的硅钢片和20#钢试件的磁畴结构,对比同种材料不同载荷试样的磁畴结构照片,分析应力对磁畴的影响。试验表明:未受力或应力集中较小时,晶粒内磁畴以片状畴为主,同一晶粒内畴壁相互平行,随着应力集中程度的增加,磁畴结构出现迷宫畴。且应力集中程度越大,迷宫畴个数越多,同时畴壁长度和间距发生改变。     

一种高效率星载电源无线能量传输系统

无接触感应电能传输技术作为一种新型的电能传输技术,具有供电安全、方便灵活的优点.本文针对磁耦合谐振式无线能量传输技术进行研究,提出一种适用于星载电源的采用串联补偿拓扑的无线能量传输系统,具体介绍功率控制和转换电路及松耦合变压器的设计;设计了一种高效率无线能量转换电路,通过建立一个220 W原理样机对系统进行验证,实际测...     

Science objectives of the magnetic field experiment onboard Aditya-L1 spacecraft

The Aditya-L1 is first Indian solar mission scheduled to be placed in a halo orbit around the first Lagrangian point (L1) of Sun-Earth system in the year 2018–19. The approved scientific payloads onboard Aditya-L1 spacecraft includes a Fluxgate Digital Magnetometer (FGM) to measure the local magnetic field which is necessary to supplement the outcome of other scientific experiments onboard. The in-situ vector magnetic field data at L1 is essential for better understanding of the data provided by the particle and plasma analysis experiments, onboard Aditya-L1 mission. Also, the dynamics of Coronal Mass Ejections (CMEs) can be better understood with the help of in-situ magnetic field data at the L1 point region. This data will also serve as crucial input for the short lead-time space weather forecasting models.The proposed FGM is a dual range magnetic sensor on a 6?m long boom mounted on the Sun viewing panel deck and configured to deploy along the negative roll direction of the spacecraft. Two sets of sensors (tri-axial each) are proposed to be mounted, one at the tip of boom (6?m from the spacecraft) and other, midway (3?m from the spacecraft). The main science objective of this experiment is to measure the magnitude and nature of the interplanetary magnetic field (IMF) locally and to study the disturbed magnetic conditions and extreme solar events by detecting the CME from Sun as a transient event. The proposed secondary science objectives are to study the impact of interplanetary structures and shock solar wind interaction on geo-space environment and to detect low frequency plasma waves emanating from the solar corona at L1 point. This will provide a better understanding on how the Sun affects interplanetary space.In this paper, we shall give the main scientific objectives of the magnetic field experiment and brief technical details of the FGM onboard Aditya-1 spacecraft.     

Analysis of a long-duration AR throughout five solar rotations: Magnetic properties and ejective events

Coronal mass ejections (CMEs), which are among the most magnificent solar eruptions, are a major driver of space weather and can thus affect diverse human technologies. Different processes have been proposed to explain the initiation and release of CMEs from solar active regions (ARs), without reaching consensus on which is the predominant scenario, and thus rendering impossible to accurately predict when a CME is going to erupt from a given AR. To investigate AR magnetic properties that favor CMEs production, we employ multi-spacecraft data to analyze a long duration AR (NOAA 11089, 11100, 11106, 11112 and 11121) throughout its complete lifetime, spanning five Carrington rotations from July to November 2010. We use data from the Solar Dynamics Observatory to study the evolution of the AR magnetic properties during the five near-side passages, and a proxy to follow the magnetic flux changes when no magnetograms are available, i.e. during far-side transits. The ejectivity is studied by characterizing the angular widths, speeds and masses of 108 CMEs that we associated to the AR, when examining a 124-day period. Such an ejectivity tracking was possible thanks to the multi-viewpoint images provided by the Solar-Terrestrial Relations Observatory and Solar and Heliospheric Observatory in a quasi-quadrature configuration. We also inspected the X-ray flares registered by the GOES satellite and found 162 to be associated to the AR under study. Given the substantial number of ejections studied, we use a statistical approach instead of a single-event analysis. We found three well defined periods of very high CMEs activity and two periods with no mass ejections that are preceded or accompanied by characteristic changes in the AR magnetic flux, free magnetic energy and/or presence of electric currents. Our large sample of CMEs and long term study of a single AR, provide further evidence relating AR magnetic activity to CME and Flare production.