行星际磁场

行星际磁场扇形结构对中低纬地磁场的影响

IMF sector effect on geomagnetic field at mid and low latitudes

行星际磁场扇形边界与地磁扰动

The Sector Boundary of IMF and the Geomagnetic Disturbance

行星际磁场By分量对地球磁层顶场向电流调制

Influence of interplanetary magnetic field b_y on the field-aligned current in the magnetopause

MD型行星际磁场螺旋扇形过渡区中的不稳定性

Instabilities in the MD Type Spiral Sector Transition Region of the Interplanetary Magnetic Field

本文采用六层模式，讨论了MD型行星际磁场螺旋扇形过渡区的稳定性。

By using a six-layer model , the stabilities of MD type spiral sector transition region in the interplanetary magnetic field are discussed .

异常SSC事件上升时间与行星际磁场方向关系不明显.L上的关系（？）

There is no explicit relation between the rise time of the anomalous SSC events and the interplanetary field direction .

我国北极黄河站全天空极光观测显示了北极极区电离层对磁层顶磁重联有很好的响应，并且发现极光增亮的区域与行星际磁场（IMF）时钟角有很强的依赖关系。

The optical aurora measurements showed that the observational ionospheric region was good response to the magnetopause reconnections . The regions of the aurora brightening were much dependent on the IMF clock angle .

离子通量的变化大体上是无色散的。离子主要受南向行星际磁场（IMF）所引起的对流电场的驱动注入到环电流区域。

Ions are injected from the magnetotail to the ring current region in a dispersionless mode most probably by enhanced convective electric field that driven by steady southward interplanetary magnetic field ( IMF ) .

本文采用球坐标下2.5维理想MHD模型，对日球子午面内方位磁场扰动的传播进行数值模拟，重点分析它对行星际磁场螺旋角的影响。

A 2.5 dimensional , ideal MHD model in spherical coordinates is used to numerically simulate the propagation of azimuthal magnetic field disturbances with emphasis upon its influence on the spiral angle of the interplanetary magnetic field ( IMF ) .

日面方位磁场扰动和行星际磁场螺旋结构

Azimuthal magnetic field disturbances and spiral structure of the interplanetary magnetic field

行星际磁场北向分量触发磁层扰动的可能性

Possibility of Triggering the Geomagnetic Disturbances by the IMF Northward Bz Component

行星际磁场的螺旋扇形过渡区

The spiral sector transition regions in the interplanetary magnetic fields

太阳耀斑和行星际磁场南向分量之间的相关分析

Cross-correlation analysis between the solar flares and the southward components of interplanetary magnetic fields

南极中山站电离层漂移特性及其对行星际磁场的响应

Ionospheric drift properties and its response to the IMF conditions at Zhongshan station , antarctica

日冕中的Ⅲ型爆发源与行星际磁场线的比较

Type ⅲ burst sources in the corona and comparisons with the interplanetary magnetic field lines

建立全球磁层三维模型后，用建立好的模型来研究行星际磁场的改变对磁层中各个物理量的改变。

After creating the magnetosphere model . We change the interplanetary magnetic field near the earth , and observe the physical quantities in the magnetosphere .

本文用典型事件和统计分析论证了行星际磁场北向分量触发地磁扰动的可能性。

The possibility of triggering the geomagnetic disturbances by the northward Bz component of the IMF is discussed using some typical events and statistical analyses .

携带着行星际磁场的太阳风被地球磁层所减速产生了弓激波以及磁鞘区。

The solar wind , carrying the plasma and IMF , is slowed down by the magnetosphere , produce the bow shock region and the magnetosheath .

主要结果是：（1）行星际磁场起伏的强度和各向异性在磁鞘中被显著放大；

The main results are : ( 1 ) the fluctuation intensity and fluctuation anisotropy of the interplanetary magnetic field are amplified obviously in the magnetosheath region ;

不同于磁层顶的磁场重联，磁鞘重联仅仅会导致行星际磁场的结构位形发生变化以及磁鞘区的等离子加热以及加速。

Unlike the magnetopause reconnection , the magnetosheath reconnection can only lead to the topology change of IMF and the acceleration and heating of the magnetosheath plasma .

在特定的行星际磁场强度下，从表面反射出来的质子有机会进入月球的夜侧半球，这是个以往被认为缺乏太阳风质子的空腔区域。

Under certain condition of the interplanetary magnetic field , a portion of them can reach the shadow region which is usually considered to be devoid of solar wind protons .

进入/撤回事件的统计结果显示，这类事件较易发生在南向行星际磁场期间，并且发生此类事件时的平均地磁活动指数比所有的磁尾电流片拍动事件要大一些。

The Enter / Retreat events show a correlation with southward interplanetary magnetic field ( IMF ), and the averaged geomagnetic index show that these events occurred under a larger value than that of the magnetotail current sheet .

行星际磁场方向对磁场起伏特性在磁鞘中的分布有强烈的控制作用，早晨侧响应灵敏，黄昏侧反响不大.相对地讲，黄昏侧的磁活动较之早晨侧稳定；

The distribution characteristics are controled strongly by the directions of the interplanetary magnetic field , the dawn-side more sensitive than the dusk-side , relatively speaking , the magnetic activity of the dusk-side is more stable than the dawn-side ;

事实上，太阳风及其所携带的行星际磁场也是地球磁层细致结构以及磁层各种物理现象的直接或间接原因。

In fact , the solar wind , as well as the IMF carried by it , could be considered as direct or indirect cause of the fine structures of magnetosphere and also the various physical phenomenons of magnetosphere .

日地关系是空间等离子体物理研究中的一个重要方面，太阳风驱动行星际磁场以及行星际的等离子体与地球偶极磁场的相互作用产生了我们所观测到的磁层。

Solar-terrestrial relation is an important aspect of space plasma research . The interplanetary magnetic field ( IMF ) and plasma , driven by the solar wind , interacts with the dipole field of the earth and generates the observed magnetosphere .

用第一特征向量推断行星际磁场的扇形极性，其符合率在两分点月份和夏季达到70%左右，冬季低于50%，暗示了冬季反向扇形效应的存在。

The first eigenvector is used to estimate IMF sector polarities . The agreement of this estimate with satellite observations is ~ 70 % in summer and equinoctial months and less than 50 % in winter , which implies the inverse sector effect in winter .

资料分析表明：南北双极讯号的出现几率远低于北南双极讯号，并且南北双极事件主要发生于行星际磁场北向和地磁宁静条件，它们往往与小的孤立的地磁亚暴相关。

The occurrence rate of the S N bipolar events is apparently lower than that of the N S events . The S N bipolar events occur primarily during quiet geomagnetic and north IMF B z conditions , and are correlated with small isolated geomagnetic substorms .

随着行星际磁场与日地连线夹角的增大，弓激波强度参数的最大值有所减小，且位置朝远离日下点方向偏移；但气压比和总压比的分布基本上不受影响。

When the angle between the IMF and the Sun-Earth line increases , the maxima of shock strength parameters of the bow shock decrease and the maximum points shift away from the subsolar point , but the distributions of gas-pressure ratio and total pressure ratio are essentially not affected .

行星际变化磁场及其对宇宙线强度的调制

Variational Magnetic Field in the Interplanetary Medium and Modulation for Cosmic-Ray Intensity

太阳宇宙线在行星际空间的传播，包括行星际不规则磁场中的扩散和太阳风对流这两种物理过程。

Physical processes of the propagation of the solar cosmic rays in the interplanetary space include the diffusion in interplanetary disordered magnetic fields and the convection in solar winds .