Case study of September 24–26, 1998 magnetic storm

We compute global magnetospheric parameters based upon solar wind data obtained from the WIND spacecraft upstream. Using the paraboloid magnetospheric model, calculations of the dynamic global magnetospheric current systems have been made. The solar wind dynamic pressure, the interplanetary magnetic field, the strength of the tail current, and the ring current control the polar cap and auroral oval size and location during the magnetic storm. The model calculations demonstrate that the polar cap and the auroral oval areas are mainly controlled by the tail current. The substorm onset at 0630 UT on September 25, 1998 happened near the minimum in the main phase field depression. The substorm expansion onset time is also marked by a sudden enhancement in the solar wind dynamic pressure and an enhancement in the tail current. The magnetic signatures of these two effects cancel each other, which explains why the D_st profile shows no strong time variation during the substorm. Evidence for the substorm expansion includes not only the signature in the AL index but also the strong asymmetry of the low latitude magnetic disturbances (substorm positive bay signature). Model calculations were checked by comparison with the GOES 8 and 10 magnetic field measurements.     

电子设备敏感机理分析

接收机、放大器的带内敏感度是用来评价设备电磁易损性的极好方法。本文介绍了敏感度指标的计算方法 ,并分析了模拟电路和数字电路的敏感机理 ,最后 ,对敏感设备的电磁兼容性设计方法进行了讨论。     

传导干扰研究

传导发射是沿电源线或信号线传输的电磁发射,在低频范围内,传导发射是电磁干扰的主要形式。如不采取措施,几乎所有的电子、电气设备电源线的传导发射都得超标,若将这些设备安装在飞机上,它将严重地威胁着机上其他设备的正常工作。本文对各种脉冲波形的频谱进行了比较,并对整流器的谐波发射进行了分析,最后介绍了降低传导发射的设计方法。     

某测试系统检查仪频率信号发生电路设计

根据研制某检查仪的任务需求，对某航空发动机转速频率信号、振动频率信号进行分析，设计了模拟相应频率信号的发生电路，用于检查仪的研制。     

电站铁磁构件早期损伤无损检测方法的研究

本文通过理论分析和实际检验，探讨了磁记忆检测地电站气轮机时片和高压缸体由应力集中引起的损伤区域进行预诊断的可靠性，并指出，该检测方法在电站实际工程检测中有良好的应用前景。     

磁壳参数L与磁暴Dst指数和行星际条件的关系

用磁坐标L-/A来描述地球近地空间粒子特性和卫星位置是近年来空间物理探测研究和数据分析中的一个新趋势.利用T96磁场模型计算了L值,并比较了在地球磁层剧烈活动期间和不同行星际条件下,用偶极子模型,国际参照磁场(IGRF)模型,和T96磁场模型这三种方式计算得到的地球表面L-A磁坐标之间的区别.在地磁纬度大于30°时偶极子近似和IGRF磁场模型计算得到的L值差别开始增大.在地磁纬度大于50°时,用IGRF磁场模型和T96磁场模型计算得到的L值差别开始增大.由于T96磁场模型引入了行星际磁场南北和东西分量,计算的L值包含了行星际条件的影响,并具有了随地方时变化的特性.本工作对于辐射带粒子动态模式的建立,以及正确理解卫星磁坐标位置等具有重要意义.     

What is the role of magnetic null points in large flares?

We have performed the analysis of the magnetic topology of active region NOAA 10486 before two large flares occurring on October 26 and 28, 2003. The 3D extrapolation of the photospheric magnetic field shows the existence of magnetic null points when using two different methods. We use TRACE 1600 Å and 195 Å brightenings as tracers of the energy release due to magnetic reconnections. We conclude on the three following points:

1. The small events observed before the flares are related to low lying null points. They are long lasting and associated with low energy release. They are not triggering the large flares.

2. On October 26, a high altitude null point is found. We look for bright patches that could correspond to the signatures of coronal reconnection at the null point in TRACE 1600 Å images. However, such bright patches are not observed before the main flare, they are only observed after it.

3. On October 28, four ribbons are observed in TRACE images before the X17 flare. We interpret them as due to a magnetic breakout reconnection in a quadrupolar configuration. There is no magnetic null point related to these four ribbons, and this reconnection rather occurs at quasi-separatrix layers (QSLs).

We conclude that the existence of a null point in the corona is neither a sufficient nor a necessary condition to give rise to large flares.     

“磁栅—光准直定位”大尺寸测量系统

介绍一种简单而又实用的大尺寸测量系统。该系统包括两个组成部分——磁栅测尺及光准直定位装置,其测量精度优于2×10~(-5)。     

Numerical study of magnetic reconnection possibly occurring near heliospheric current sheet

The third-order accurate upwind compact difference scheme has been applied for the numerical study of the magnetic reconnection driven by a plasma blob impacting the heliospheric current sheet, under the framework of the two-dimensional compressible magnetohydrodynamics. The results show that the driven reconnection near the current sheet could occur in about 10–30 min for the interplanetary high magnetic Reynolds number, R_M = 2000–10,000, a stable magnetic reconnection structure can be formed in hour order of magnitude, and there appear some basic properties such as the multiple X-line reconnections, vortex structures, filament current systems, splitting and collapse of the high-density plasma blob. These results are helpful in understanding and identifying the magnetic reconnection phenomena possibly occurring near the heliospheric current sheets.     

大功率晶体管最优驱动电路研究

大功率晶体管深度饱和以降低功率损耗与管子快速关断之间的矛盾并非不可调和。文中针对通常的抗饱和驱动，提出了一种新型驱动电路，很好地解决了这个矛盾。一方面在功率管饱和导通时，比例驱动管子工作于深饱和状态，使功率管的损耗达到最小；另一方面在功率管关断时，驱动电路通过低阻抗抽流回路及高反压辅助抽流的引入，在功率管的基极提供很强的基极反抽电流，使管子快速关断。实验表明与通常的抗饱和驱动相比，本方案由于功率管深度饱和，从而使管子的通态饱和压降降低了0.5V，损耗亦降低了63.4W；另一方面由于关断时基极反抽电流增大了三倍，存储时间增加权0.1us，实现了大功率晶体管的最佳驱动。