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首页> 外文期刊>Journal of Geophysical Research, A. Space Physics: JGR >Statistical characteristics of the storm time plasma sheet
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Statistical characteristics of the storm time plasma sheet

机译：风暴的统计特征等离子体片

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The present study addresses the convection and configuration of the storm time plasma sheet by examining the occurrence ratios of fundamental plasma quantities. Measurements made by the Geotail spacecraft in the midnight sector are used. The results are summarized as follows: (1) the occurrence ratio of the plasma flow velocity is not noticeably different between storm and nonstorm time or between the main and recovery phases; (2) the convection electric field is more intense during the main phase; (3) the equatorial magnetic field is stronger during the main phase; (4) the ion pressure is higher, therefore the tail current is more intense, during the main phase. It is suggested that the stronger equatorial magnetic field (result 3) counteracts the enhancement of the convection electric field (result 2) so that the occurrence ratio of the flow velocity does not depends on geomagnetic activity (result 1). The storm time increase in the equatorial magnetic field can be attributed to the X-dependent intensification of the dawn-to-dusk electric current (the ring current and tail current); if the current is more intensified on the earthward side than on the tailward side, the net change in B Z is positive. It is also found that the reconnection takes place, if infrequently, at X > ?15 R E during storm periods. However, result 1 suggests that despite the intense tail current (result 4), the X distribution of the near-Earth reconnection site does not statistically depend on storm activity. This can also be attributed to the stronger equatorial magnetic field as well as to the storm time enhancement of the near-Earth plasma number density. It is therefore suggested that the ring current affects the plasma sheet dynamics through its contribution to the tail magnetic configuration.
机译：本研究解决了对流风暴时间等离子体片的配置检查基本的发生比率等离子体的数量。Geotail航天器在午夜部门使用。等离子体流的发生比速度风暴,之间并没有明显的区别nonstorm之间的时间或主要和恢复阶段;强烈的主要阶段;磁场强的主要阶段;(4)离子压力较高,因此尾电流更强烈,在主要的阶段。赤道磁场(结果3)抵消对流电场的增强(2)结果的发生比率流速不取决于地磁活动(1)结果。暴风雨时间增加赤道磁场可以归结的X-dependent集约化黎明到黄昏电流(电流环和尾电流);向地球的一面而不是加剧tailward方面,B Z的净变化是积极的。还发现,重新连接的地方,如果很少,在X > ? 15 R E期间风暴期。尽管激烈的尾电流(4)结果,X分布的近地重新连接网站统计上并不依赖于风暴活动。更强的赤道磁场以及暴风雨时间增强近地等离子体密度。环电流影响等离子体单动力学通过其贡献的尾巴磁配置。

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