双极型磁选态单束铯束管内铯原子运动轨迹的算法改进

针对简化算法得到的铯原子运动轨迹精度不高的结果,通过分析磁选态单束铯束管内双极型选态磁铁的磁场分布,提出了不简化磁场梯度和有效磁矩,用布利厄施-施多厄方法求解铯原子运动方程的算法。用此算法得到的铯原子运动轨迹与通常采用的简化算法得到的轨迹相比,最大差异约为10 mm。此计算结果影响管内机械组件的安装对中位置,可用于束光学模拟计算,提高短期稳定度指标。     

Evolution of coronal mass ejection/shock system in interplanetary space

The evolution of coronal mass ejection/shock system is investigated by numerically solving the usual set of two-dimensional single-fluid polytropic magnetohydrodynamic equations from 1 R_s to 1 AU in the meridian plane. The simulation result reveals that the coronal mass ejection/shock system formed near the sun evolves into the magnetic cloud/shock system near the earth’s orbit through the following three phases: the initial formation, the dominant latitudinal expansion and the similar expansion.     

Relativistic solar protons in the ground level event of 23 February 1956: New study

In this study we applied again to the outstanding solar particle event of 23 February 1956, the largest one in the entire history of observations of solar cosmic rays. Due to significant improvement of the analysis/modeling techniques and new understanding of physical processes in the solar atmosphere and interplanetary space, a possibility arises to interpret the old data in the light of modern concept of multiple particle acceleration at/near the Sun. In our new analysis the data of available then neutron monitors and muon telescopes are used. The technique of the analysis includes: (a) calculation of asymptotic cones of ground-based detectors; (b) modeling of cosmic ray detector responses at variable parameters of the flux of solar relativistic protons; (c) determination of primary solar proton parameters outside magnetosphere by comparison of computed responses with observations. Certain evidence was obtained that the flux of relativistic solar protons consisted of two distinct components: prompt and delayed ones. The prompt component with exponential energy spectrum caused a giant impulse-like increase at a number of European cosmic ray stations. The delayed component had a power-law spectrum and was a cause of gradual increase at cosmic ray stations in the North American region. A numerical simulation of the proton acceleration in the vicinity of the magnetic reconnection region brings to the proton spectrum with exponential dependence on energy. This agrees with observational data for the prompt component. It is also shown that the huge increase in ∼5000% on neutron monitors was due to the prompt component only with the exponential proton spectrum. The power-law spectrum of comparable intensity gave considerably smaller effect.     

磁尾等离子体片对流对亚暴的影响

采用2(1/2)维全粒子电磁模拟方法研究了等离子体片中稳态对流及局地爆发高速流对磁层亚暴触发过程的影响.研究发现,地向瞬时局地高速流可触发磁场重联,导致储存于磁尾磁场能量的快速释放.但是,等离子体片稳态对流可抑制磁尾磁场重联过程.此项研究结果表明,局地爆发高速流能够触发磁层亚暴;而行星际磁场(IMF)持续南向时的稳态磁层对流期间,不易发生亚暴.      

利用地磁场给飞轮卸载的新方法

通过对圆轨道地磁场强度的变化规律分析 ,将卫星磁力矩器产生的磁矩按傅立叶级数展开 ,根据卫星所需卸载角动量大小 ,按照最优控制理论求出三轴磁矩取值 ,得出飞轮卸载控制律。最后文章给出飞轮卸载稳定性分析和仿真结果 ,表明这种飞轮卸载方法简单而且省能量。     

Temporal evolution analysis of storm-enhanced density during an intense magnetic storm on March 2015

An intense Storm Enhancement Density (SED) event with the magnetic storm occurred on 17–24 March 2015 has been investigated. The morphological character of the SED during different phase of the magnetic storm is examined and compared with the non-storm time. Three intensity indexes, i.e., “general” SED index, “heavy” SED index and “severe” SED index, are defined to represent the intensity of SED respectively represented by the numbers of the ionospheric total electron content (TEC) grids with TEC > 60 TECu, TEC > 80 TECu and TEC > 100 TECu. The temporal evolution of the SED intensity indexes during a time span covering the non-storm time and the magnetic storm time have also been investigated. The SED exhibits a shape with two parallel slender troughs in the middle and low latitudes during the non-storm time and then gradually develops into an ellipse structure as the development of magnetic storm. The intensity of SED and the fluctuation of the TEC evolution are generally corresponding to the fluctuation of Dst index. The analyzing results enrich our understanding of the temporal and spatial evolution of the ionospheric SED.     

Compensation of time-variable magnetic moments for a precise attitude control in nano- and micro-satellite missions

Theses days, many nano- and micro-satellites are applied to several astronomy and remote sensing missions. In order to achieve mission requirements, these satellites must control the attitude precisely. A magnetic disturbance is one of the dominant sources of attitude disturbances. Therefore, this disturbance should be canceled in-orbit or on the ground to achieve the attitude strict requirements. This paper presents the effect of the magnetic disturbance to the attitude in nano- and micro-satellite missions and the sources of the residual magnetic moment of the satellites, which causes the magnetic disturbance. Then, the paper proposes a method to compensate the residual magnetic moment both in-orbit and in the design phase of the satellites. The research also focused on a time-varying residual magnetic moment. Finally, the method is applied to a micro-astrometry satellite as an example.     

The role of vorticity in 3D magnetic field annihilation

We show that magnetic field annihilation depends strongly on the behaviour of the vorticity and is quite different in 2D and 3D. In 3D the vorticity can be increased locally by the stretching of vortex lines (an effect that is absent in 2D). This leads to the onset ofcellular flow at quite low vorticities and the fragmentation of the simple current sheet.     

Modeling the coronal magnetic field in a polar hole

The coronal magnetic field in the northern polar coronal hole in 1986 is predicted on the basis of the photospheric magnetic field observations and the horizontal current-current sheet coronal model (Zhao and Hoeksema, 1993). The predicted magnetic field intensity is stronger near the center of the hole than near the edge. The calculated expansion factor for the entire hole does not match the expansion factor of any flux tube in the hole, suggesting that it would not be appropriate to use the expansion factor for entire hole to represent the divergence of the flux tube in analyzing the acceleration and heating of the plasma in coronal holes.     

连续分离铝熔体中夹杂物的分析

通过分析高频磁场作用下熔体连续处理时夹杂的去除效率表明，熔体连续处理条件下的夹杂去除效率比熔体静止时的略低，而夹杂与熔体之间的密度差对电磁分离时的去除效率影响不大。提高去除效率的有效途径是增大磁感应强度或降低分离器管径，但减小管径的同时需要提高磁场频率，以保持α/δ的值在2附近才可以取得最佳的分离效果。