Solar and interplanetary origins of the November 2004 superstorms

During the first half of November 2004, many solar flares and coronal mass ejections (CMEs) were associated with solar active region (AR) 10696. This paper attempts to identify the solar and interplanetary origins of two superstorms which occurred on 8 and 10 November with peak intensities of Dst = −373 nT and −289 nT, respectively. Southward interplanetary magnetic fields within a magnetic cloud (MC), and a sheath + MC were the causes of these two superstorms, respectively. Two different CME propagation models [Gopalswamy, N., Yashiro, S., Kaiser, M.L. et al. Predicting the 1-AU arrival times of coronal mass ejections. J. Geophys. Res. 106, 29207–29219, 2001; Gopalswamy, N.S., Lara, A., Manoharan, P.K. et al. An empirical model to predict the 1-AU arrival of interplanetary shocks. Adv. Space Res. 36, 2289–2294, 2005] were employed to attempt to identify the solar sources. It is found that the models identify several potential CMEs as possible sources for each of the superstorms. The two Gopalswamy et al. models give the possible sources for the first superstorm as CMEs on 2330 UT 4 November 2004 or on 1454 UT 5 November 2004. For the second superstorm, the possible solar source was a CME that on 0754 UT 5 November 2004 or one that occurred on 1206 UT 5 November 2004. We note that other propagation models sometimes agree and other times disagree with the above results. It is concluded that during high solar/interplanetary activity intervals such as this one, the exact solar source is difficult to identify. More refined propagation models are needed.     

On the motions of RHESSI flare footpoints

The footpoint motions of flare hard X-ray (HXR) sources are directly related to the reconnection scenario of a solar flare. In this work, we tried to extract the information of footpoint motions for a number of flares observed with RHESSI. We found that the RHESSI flare results of the footpoint motions strongly support the classification proposed from the observations of YOHKOH/HXT. Furthermore, it is found that a flare can consist of two types of footpoint motions. We discussed the connections of the footpoint motions with the two-dimensional reconnection models.     

Electron temperature anisotropy effects on tearing mode in ion-scale current sheets

Recent two-dimensional (2-D) particle-in-cell (PIC) simulations have shown that there is a critical thickness of a current sheet, above which no significant saturation amplitude of the 2-D tearing (TI) mode can be expected. Here, we have introduced the initial electron temperature anisotropy (α_e0 = T_e⊥/T_e|| > 1), which is known to raise significantly the linear growth rates, and inspected if α_e0 > 1 can change the saturation level of the TI in a super-critical current sheet. Varying α_e0 and D (D: the current sheet half-thickness) systematically, we have found that while α_e0 boosts up the linear growth rate in both sub- and super-critical current sheets, macroscopic effects are obtained only in sub-critical current sheets, that is, energy transfer from the fastest growing short wavelength modes to longer wavelength modes are available only in the sub-critical regime. Since the critical thickness is a fraction of the ion inertial length, the tearing mode assisted by the electron temperature anisotropy alone, despite its significant boost in the linear growth rate, cannot be the agent for reconnection triggering in a current sheet of ion-scale thickness.     

空间微重力磁悬浮平台激励器研究

为满足空间实验室的科学实验载荷对微重力环境水平的要求,需要保证空间微重力实验载荷平台的振动隔离性能,即需要平台激励器能在控制系统的作用下适时地产生抑制平台扰动的激励力.本文提出了平台激励器的初步指标,从磁悬浮基本原理出发设计出多种结构形式,在此结构基础上完成有限元磁路仿真和激励器的线圈设计,并对各种结构形式进行比较,根据比较结果总结出各结构形式的优缺点,为激励器的具体设计提供了依据.      

磁扰期间的三维漂移壳分离

基于磁层粒子动力学理论,首先对比了计算漂移壳分离的引导中心法和磁力线追踪法,计算表明两种方法的计算结果一致.然后分别采用T89c和T96磁层磁场模式,用磁力线追踪法数值计算了不同初始位置(≤9Re)、不同初始投掷角、不同Kp指数和不同太阳风压力下,带电粒子的漂移壳分离.计算结果揭示了漂移壳分离随初始位置、投掷角、Kp指数和太阳风压力的变化.其具体特征如下. (1)随着径向距离的增大,漂移壳分离效应愈加显著,由正午出发的粒子将被稳定捕获,而午夜出发的径向距离≥7Re的部分大投掷角粒子将沿磁层顶逃逸. (2)正午出发的粒子,漂移到午夜时其漂移壳随投掷角减小向外排列;午夜出发的粒子,漂移到正午时其漂移壳随投掷角增大排列; 90°投掷角粒子在磁赤道面的漂移壳沿着磁场等值线排列. (3)漂移壳分离随Kp指数和太阳风压力增大变得显著,且随这两种扰动参数的变化特征和趋势是基本相似的.      

Influence of different atmospheric models and seeing effects on the nonlinear calibration

This paper describes a technique intended to improve calibration of vector magnetograms achieved by the spectral line Fei 5324.19 Å which was first described in detail by Hagyard and Kineke [Hagyard, M.J., Kineke, J.I., Improved method for calibrating filter vector magnetographs, Solar Phys., 158, 11–28, 1995.]. The technique attempts to compensate for nonlinear behavior of the measured linear and circular polarizations of the line as functions of inclination angle and field strength. This method depends on different atmospheric models. To the three different atmospheric models, the VAL-C quiet photosphere model, the Ding and Fang penumbra model and Allen umbral model, the circular polarization signal is directly linearly proportional to the longitudinal field strength in the range of 800 G, 1000 G and 1300 G, respectively. For the transverse field, however, this linear relationship holds over much smaller ranges which are 200 G, 300 G and 200 G. The improved method improves the accuracy in calibrating the polarization signals over a wide range of field strengths and inclination angles. With the seeing effects decreasing in the magnetic observation, the longitudinal fields and the transverse ones are underestimated. The differences in the zero-iterative longitudinal and transverse field are relatively minor, but differences in the multi-iterative longitudinal and transverse field can be as high as 260 G and 500 G. The improved calibration method is more sensitive to the seeing effects variation than the former calibration method.     

On geomagnetic variations during the August–September storms of 1859

Hourly magnetic readings of H and D from six geomagnetic observatories in Finland and Russia were utilized for analysis of the time behavior of the extreme space weather event of August/September 1859. The observatories cover about 200° in longitude and magnetic latitudes 45–60°N.     

万向磁悬浮动量轮研究

目前大部分空间飞行器三轴姿态控制采用的是飞轮系统 ,其精度较高 ,而采用磁悬浮轴承支承的动量轮比普通的滚珠轴承动量轮有更高的姿控性能。在此基础上发展的动量矩方向可改变的万向磁悬浮动量轮可以单独实现三轴较高精度的主动姿态控制 ,具有重要的实用价值。同时 ,万向磁悬浮动量轮的研究也为集成能源与姿态控制系统的研究提供了技术支持。文意介绍了万向磁悬浮动量轮在国际上研究和发展的情况 ,概括了其中的关键技术 ,并给出了一种初步的结构设计实例。     

FY—1C卫星空间粒子成分监测器及其探测结果

简要介绍了FY－1C星空间粒子成分监测器的任务目标、工作原理、创新特色及在轨探测结果。空间粒子成分监测器用于卫星轨道空间的带电粒子辐射监测，为卫星的在轨安全和抗辐射加固设计服务。监测器在世界上实现用1套传感器完成对高能电子、质子、α粒子至铁离子的全成分监测，使我国首次获得了870km高太阳同步轨道全空间的各种重离子分布、质子能谱分布和电子通量分布，捕捉到大量的地磁暴和太阳质子事件，获得了批重要的探测成果。     

磁选态单束铯束管铯原子速率分布的模拟计算

对铯炉准直器出口铯原子束的速率分布和角分布进行抽样,用蒙特卡罗方法模拟计算磁选态单束铯束管中五个关键位置的铯原子不同能级态的速率分布。结果是检测器处的铯原子速率分布不再符合麦克斯韦分布,分布密度最大值对应速率不随铯炉温度改变,只和束光学设计的参数有关。此模拟计算对指导磁选态铯束管束光学的设计有较大帮助。