信使号再次飞探水星

6月2日,美国航宇局科学家发布消息说,根据信使号航天器丙次飞掠水星所进行的探测,太阳风可能是水星大气层不断得到科技支农补充的重要原因.     

Pc5 Oscillation Analysis by the Satellite and Ground-Based Data

Large amplitude Pc5 event was observed in the space and on ground on August 3, 2001, about three hours after contact of the strong discontinuity in the solar wind with the magnetosphere according to data from ACE and Wind satellites. The Pc5 amplitude was as high as 15 nT in the tail of magnetosphere and about 5 nT at the ground based stations. In the magnetosphere Pc5 waves were observed by Cluster and Polar satellites, which occupied positions in the morning part of the near tail at the close field lines but were parted by distance of 11.5 Re, mainly along the x-axis of the GSM coordinate system. Both compressional and transverse components of the Pc5 wave activity were observed in the space, with the transverse component having the larger amplitude. Time delay between the Cluster and Polar satellites was about 8 minutes, which could be interpreted as a wave propagation from the geomagnetic tail to the Earth with the 150 km/s group velocity. The ground-based Pc5 activity was analysed by using data from the Image magnetometer network. Doubtless demonstrations of a field line resonant structure were found in variations of amplitude and polarization with latitude. Finnish chain of search coil magnetometers observed modulated Pc1 emission simultaneously with the Pc5 wave train. A possibility of non-linear impact of Pc5 wave energy on the plasma and waves in the magnetosphere is discussed.     

A Theoretic Interpretation of Movement of the Cusp Equatorward Boundary

A preliminary model is proposed to describe quantitatively the position and movement of cusp equatorward boundary. This integrated model, consisting of an empirical model of the magnetopause and a compressed dipolar model of Open/Closed field line, connects quantitatively the solar wind conditions, subsolar magnetopause and cusp equatorward boundary. It is shown that the increasing solar wind dynamic pressure and the increasing southward Interplanetary Magnetic Field (IMF) component drive the magnetopause to move inward and the cusp equatorward. This model is adopted to interpret quantitatively the cusp movement of August 14, 2001 observed by Cluster. The results show that the subsolar magnetopause moved earthward from 10.7 He to 9.0 Re during the period of 002300-002800 UT, and correspondingly the cusp equatorward boundary shifted equatorward. The observations of Cluster C1 and C4 show the cusp equatorward boundary that Cluster Cl and C4 were crossing during same interval moved equatorward by 4.6°. The cusp equatorward boundary velocity computed in the theoretical model (10.7km/s) is in good agreement with the observed value (9.4km/s) calculated from the data of CIS of Cluster C4 and C1.     

行星际强磁场结构中的亚阿尔文波速流

1982年11月23日开始的极高速太阳风流追赶强磁场结构的事件,形成了高密度前鞘-强磁场本体-高密度后鞘-高速流的组合结构。本文分析了此组合结构的磁流体动力学特征,发现在强磁场本体内出现行星际亚阿尔文波速流,并推论了其可能的成因。      

关于IMF北向分量特强时的太阳风－磁层－电离层耦合

Relationship between the solar wind-magnetosphere energy coupling function and the energy consumption in the magnetospheric system is tested by the samples during period of northward B_z(>10 nT) of IMF. It is shown that the energy function which can well describe the solar wind-magnetosphere coupling when B_z>0 is no more applicable for B_z>10 nT, but the coupling still exists, the effects of which are mainly found at the polar cap. Dst often turns to positive when B_z> 10 nTand the coupling mechanism is different from that when B_z<0. New coupling function has to be introduced to describe the solar wind-magnetosphere coupling for the case of B_z> 10 nT.      

二维磁流体动力学平衡日冕(Ⅱ)

基于解析和数值相结合的方法,进一步讨论了非均匀引力场中日冕的二维磁流体动力学平衡。对临界点进行了比较仔细的处理。得到了包含闭场区、中性片和开场区的大尺度日冕磁场位形,闭场区和中性片构成冕流结构。在高纬和低纬地区几个太阳半径之外,等离子体径向流动速度超过了局地声速和局地Alfvén速度。在1AU处,太阳风速度可达到400kms_-1以上      

日冕扰动传播的数值模拟(Ⅲ)太阳风的影响

本文数值研究了二维磁流体动力学平衡基态下开场区日面冷物质径向喷射所引起的日冕动力学响应。结果表明:(1)在高密度环前方有一弱扰动区近似以Alfvén速度向外传播;(2)高密度环前缘移动速度随着径向距离而增加, 其增加值近似为局地太阳风速度;(3)高密度环中等离子体的最大径向速度约在4个太阳半径处趋于局地逃逸速度;(4)对于强开放场, 环形结构在θ方向上没有明显的扩张。这些结果可以更好地解释伴随有日珥的日冕物质抛射事件。      

I型彗尾风差角的分析及其所显示的太阳风的传播特性

文章分析了I型彗尾风差角的大量资料, 得出其变化和日心距离的关系是不大的;但对日心黄纬, 却显示出逐渐减小的趋向.文章还得出, 风差角的变化随着彗星的切向速度而单调上升, 从而进一步证实了动力风差原理是形成风差角的主要因素.在此基础上, 分析了太阳风速度场的分布特性, 得出了平均太阳风速度随日心距离的变化是不明显的, 而随日心黄纬有着缓慢增强的趋势.      

太阳风粒子速度分布不对称性的产生机制

1引言太阳风中由于磁场的作用,在垂直磁场平面内质子做回旋运动．通常在此平面的质子速度分布函数是旋转对称的．实际观测中,虽然大部分由测量值内插得到的速度分布是旋转对称的,但少数是不对称的．产生这种不对称性的原因还不清楚．文献川提出o粒子与间断面相互作用可产生非回族对称分布．由于这种非旋转对称的速度分布应是不稳定的,因而会很快弛豫到了旋转对称的分布．很难解释非对称的分布可经常被观测到的事实．我们认为这种非对称分布的观测结果并不一定是真实的非回旋对称的分布函数产生的而可能是由于太阳风等离子体小尺度的不均…     

太阳风对太阳自转减速的影响

本文研究了由于太阳风作用在太阳表面上的力矩以及太阳风造成的质量损失使太阳自转角速度减速的影响;推出了由于这些原因使自转角速度的相对改变率以及自转角速的长期改变的表达式;最后估计了自转角速减慢的相对改变率值和在一千万年内角速的长期减速值,并绘出了减速曲线。计算表明。质量损失对于相对改变率的影响可以略去,但对于长期减速的影响不应该略去。