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.     

Study of TEC changes during geomagnetic storms occurred near the crest of the equatorial ionospheric ionization anomaly in the Indian sector

GPS satellites data obtained at Bhopal (23.16° N, 77.36° E, geomagnetic latitude 14.23° N) India were analyzed to study the TEC changes during several geomagnetic storms (−300 nT < Dst < −50 nT) occurred in 2005–2007. We had segregated the storms according to the Dst value, i.e. moderate storms (−100 nT < Dst ? −50 nT), strong storms (−150 nT < Dst < −100 nT), and severe storms (Dst less than −150 nT). Total of 21 geomagnetic storms (10 moderate, 9 strong, 2 severe) are considered for the present study. Deviation in vertical total electron content (VTEC) during the main phase of the storm was found to be associated with the prompt penetration of electric field originated due to the under-shielding and over-shielding conditions for almost all geomagnetic storms discussed in this paper. For most of the storms VTEC shows the positive percentage deviation during the main phase while it shows positive as well as the negative deviation during the recovery phase of the storms. The −80% deviation in VTEC was found for geomagnetic storm occurred on July 17, 2005 and the negative trend continued for recovery phase of the storm. This was mainly due to the thermospheric composition changes by Joule heating effect at auroral latitudes that generate electric field disturbance at low latitudes. Traveling ionospheric disturbances (TIDs) were responsible for the formation of wave like nature in VTEC for the storms occurred on May 15, 2005, whereas it was not observed for storm occurred on August 24, 2005.     

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.     

关于域F上的向量空间V的一个性质的证明

利用扩张域论述方法，证明域Ｆ上的向量空间Ｖ的一个基本性质，即在Ｆ上，Ｖ关于Ｆ的基底的元数等于维数（Ｖ：Ｆ）。     

计算空气动力学的流场和图形显示技术

本文阐述了计算空气动力学流场和图形显示的重要性,它的基本方法和主要内容;介绍了在VAX计算机上研制的计算空气动力学流场和图形显示软件的主要功能。     

A Self-Consistent Determination of the Temperature Profile and The Magnetic Field Geometry in Winds of Late-Type Stars

Cool giant and supergiant stars generally present low velocity winds with high mass-loss rates. Several models have been proposed to explain the acceleration process of these winds. Although dust is known to be present in these objects, the radiation pressure on these particles is uneffective in reproducing the observed physical parameters of the wind. The most promising acceleration mechanism cited in the literature is the transference of momentum and energy from Alfvén waves to the gas. Usually, these models consider the wind to be isothermal. We present a stellar wind model in which the Alfvén waves are used as the main acceleration mechanism, and determine the temperature profile by solving the energy equation taking into account both the radiative losses and the wave heating. We also determine, self-consistently, the magnetic field geometry as the result of the competition between the magnetic field and the thermal pressure gradient. As the main result, we show that the magnetic geometry presents a super-radial index in the region where the gas pressure is increasing. However, this super-radial index is greater than that observed for the solar corona.