Cluster星簇对中磁尾尾瓣持续磁重联观测研究

当行星际磁场持续南向时, 磁尾尾瓣区积蓄大量的磁能, 出现强的晨昏电场. 此时中磁尾磁重联进行得深入持久, 在等离子体片闭合磁场和等离子体被带出重联区之后, 尾瓣区的磁场和等离子体不断进入重联区, 这种重联过程称之为“持续尾瓣重联”(CLR). 分析2001~2003年期间欧空局Cluster星簇对中磁尾的观测数据, 发现CLR除导致磁场形态改变和产生高速流外, 重联区出现空泡, 多数空泡中等离子体密度和温度下降两个数量级(少数为一个数量级). 空泡结束后, 密度较重联前低, 温度略有升高. CLR的持续时间一般为几十分钟, 它同行星际磁场持续南向发生的强亚暴有很好的相关性.     

地球磁尾两种不同类型磁结构形成机理

观测表明，横越磁尾等离子体片和尾瓣的磁场By分量正比于行星际磁场By分量，并且行星际磁场与等离子体团内By分量极性相同，因此磁尾等离子体团应该是一个三维结构。以两类磁静平衡解为初态。对亚暴期间磁尾动力学过程作二维三分量模拟研究。数值结果展示了By分量两类不同的演化特征，它们分别与具有通量绳核心的磁结构及类似于“闭合环”等离子体团型磁结构相对应。由此认为，亚暴期间在地球磁尾中出现不同拓扑位形的磁结构可能与具有不同By分量分布形态的磁场重联有关。     

磁暴和亚暴的理论预报模式

在理论研究和数据分析研究上,建立了磁暴和磁层亚暴的等效电路模式,用于预报亚暴和磁暴的指数。其输入条件为１ＡＵ处地球磁层位置的太阳风参量,模拟计算不同行星际条件下磁层和电离层系统的电流分布演化,亚暴和磁不ＡＥ和Ｄｓｔ指数变化。     

磁层亚暴过程中高速流分布

采用实际的磁尾位型,利用数值模拟方法研究磁层亚暴过程中高速流分布。结果表明垂直磁场的高速流主要分布在电流片内,范围在|Z|<0.25RE;平行磁场高速流分布区域在两个区域较大,一个是距离地球较近的磁场较强的区域,另一个是距离等离子体片较近磁场较强的区域。     

亚暴期间场向电流的特征

分析了由ISEE-1和ISEE-2飞船在亚暴期间观测到的场向电流的特性,包括场向电流所伴随的行星际磁场、地方时与L值分布以及场向电流强度和密度随亚暴位相的变化,并着重分析了亚暴电流楔的特征。结果表明,亚暴膨胀相的场向电流强度和密度都达到极大值;亚暴的膨胀相是由行星际磁场转向或南向分量变小触发的,其起始位置很可能位于近地等离子体片内边缘。     

Observations of thermospheric vector wind over Yellow River Station during auroral substorm events

Strong disturbances associated with auroral substorms originate from the ionosphere-magnetosphere owing to the effects of the solar wind, and the wind field in the ionosphere is related to such substorm activity. Here, we describe the analysis of four auroral substorm events, for which we employed an all-sky Fabry-Perot interferometer to observe the two-dimensional horizontal wind field and combined the results with data from an all-sky charge-coupled device imager, a fluxgate magnetometer installed at Yellow River Station, and the Super Dual Auroral Radar Network. The results demonstrate that, during auroral substorms, the vector wind field is related closely to variations in the ion drift and geomagnetic field. Moreover, we observed a changing wind field of approximately 300 rn/s in response to variations in the electric and magnetic fields （likely caused by ion drag） and a disturbance of about 200 m/s that we attribute to the interaction of Joule heating and ion drag.     

Pressure gradient evolution in the near-Earth magnetotail at the arrival of BBFs

Using in situ observations from THEMIS A, D and E during the 2008-2011 tail season, we present a statistical study of the evolution of pressure gradients in the near-Earth tail during bursty bulk flow （BBF） convection. We identified 138 substorm BBFs and 2,197 non-substorm BBFs for this study. We found that both the pressure and the Bz component of the magnetic field were enhanced at the arrival of BBFs at the spacecraft locations. We suggest that the increase of Bz during non-substorm BBFs is associated with flux pile-up. However, the much stronger enhancement of Bz during substorm BBFs implies the occurrence of magnetic field dipolarization which is caused by both the flux pile-up process and near-Earth current disruption. Furthermore, a bow-wave-like high pressure appears to be formed at the arrival of substorm BBFs, which is responsible for the formation of region-1-sense FACs. The azimuthal pressure gradient associated with the arrival of substorm BBFs lasts for about 5 min. The enhanced pressure gradient associated with the bow wave is caused by the braking and diversion of the Earthward flow in the inner plasma sheet. The results from this statistical study suggest that the braking and azimuthal diversion of BBFs may commonly create azimuthal pressure gradients, which are related to the forrnation of the FAC of the substorm current wedge.     

极光亚暴对太阳风压强激波的响应

研究了Polar对ISTP卫星观测的两个极光亚暴事件，此两事件与日冕物质抛射相关的太阳风压强微波到达地球有关。提出太阳风压强激波经过地球时，沿途冲击磁层顶激发磁流体快波，快Alfven波横越具有较高局地Alfven速度的磁尾尾瓣，将压缩效应迅速传递到内磁层及等离子体片，在1－2min内建立起强越尾电流，进而触发磁层亚暴。     

磁层亚暴膨胀相的协同性模型

用一元磁流体力学广义行波展开法进一步研究了近磁愉内边界的位不稳定性。将笔者以前关于近磁尾赤道面附近的漂移气球模不稳定性工作推广到非赤道区和存在非定常地向流的情形。论证了减切地向流将导致近磁尾内边界绝对不稳定，并使增长率显著增加。     

2000年4月6日磁暴夜侧场向电流变化特征

利用全球地磁台站观测数据,研究了2000年4月6日超级磁暴期间北半球夜侧场向电流变化特征.结果表明,磁暴主相期间,北半球夜侧中纬地区呈现东向磁扰的主要特征,子夜后扇区东向磁扰强于子夜前扇区.这表明夜侧高纬电离层的场向电流以流出电离层为主,流出电离层的场向电流中心在子夜后扇区,靠近子夜,即Ⅱ区场向电流和部分环电流体系在磁暴主相期间向昏侧偏转.磁层亚暴对夜侧流出电离层的场向电流有一个先减弱后增强的效应.磁暴主相期间部分环电流和Ⅱ区场向电流的发展与子夜后-晨侧扇区的西向电集流增强相对应.