Corotating solar wind streams and recurrent geomagnetic activity: A review
Corotating solar wind streams and recurrent geomagnetic activity: A review
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DOI：
10.1029/2005ja011273
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发表时间：
2006-07
影响因子：
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通讯作者：
B. Tsurutani;W. Gonzalez;A. Gonzalez;F. Guarnieri;N. Gopalswamy;M. Grande;Y. Kamide;Y. Kasahara-
中科院分区：
文献类型：
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作者：
B. Tsurutani;W. Gonzalez;A. Gonzalez;F. Guarnieri;N. Gopalswamy;M. Grande;Y. Kamide;Y. Kasahara-
[1]从太阳冕洞发出的太阳风快速流导致地球上经常性的中等强度的地磁活动。强磁场区域称为共旋相互作用区域或CIR，是由快流与上游慢流的相互作用产生的。由于CIR内的GSM磁场z分量的高度振荡性质，所产生的磁暴通常仅在强度上是弱到中等的。CIR产生的磁暴主相强度Dst < −100 nT（大磁暴）是罕见的。延长风暴“恢复”阶段的特点是连续AE活动，可以持续长达27天（太阳旋转）是由非线性阿尔芬波在高流适当。与阿尔芬波向南分量（GSM）相关的磁重联是太阳风能量传输机制。相对论电子的加速发生在这些磁暴的“恢复”阶段。与阿尔芬波相关的磁重联导致等离子体片等离子体连续、浅注入磁层。不对称等离子体对于波（合唱和其他模式）的增长是不稳定的，这是许多电子加速理论的核心特征。值得注意的是，连续的AE活动不是一系列的亚暴扩展阶段。参数也提出了为什么这些AE活动间隔不是对流海湾。在这些连续的AE活动间隔期间的极光强度低于亚暴极光，并且在性质上是全球性的（昼侧和夜侧）。由于这一活动的连续性，在太阳活动周期的大幅度下降阶段，输入磁层/电离层系统的平均能量可能比在太阳活动极大期时更大。与行星际阿尔芬波相关的不连续性和磁衰减（MD）可能对地磁活动很重要。总之，它将表明，与高速流/CIR相关的磁暴将有相同的初始，主要和“恢复”阶段与ICME相关的磁暴，但行星际的原因是相当不同的。
[1] Solar wind fast streams emanating from solar coronal holes cause recurrent, moderate intensity geomagnetic activity at Earth. Intense magnetic field regions called Corotating Interaction Regions or CIRs are created by the interaction of fast streams with upstream slow streams. Because of the highly oscillatory nature of the GSM magnetic field z component within CIRs, the resultant magnetic storms are typically only weak to moderate in intensity. CIR-generated magnetic storm main phases of intensity Dst < −100 nT (major storms) are rare. The elongated storm “recovery” phases which are characterized by continuous AE activity that can last for up to 27 days (a solar rotation) are caused by nonlinear Alfven waves within the high streams proper. Magnetic reconnection associated with the southward (GSM) components of the Alfven waves is the solar wind energy transfer mechanism. The acceleration of relativistic electrons occurs during these magnetic storm “recovery” phases. The magnetic reconnection associated with the Alfven waves cause continuous, shallow injections of plasma sheet plasma into the magnetosphere. The asymmetric plasma is unstable to wave (chorus and other modes) growth, a feature central to many theories of electron acceleration. It is noted that the continuous AE activity is not a series of substorm expansion phases. Arguments are also presented why these AE activity intervals are not convection bays. The auroras during these continuous AE activity intervals are less intense than substorm auroras and are global (both dayside and nightside) in nature. Owing to the continuous nature of this activity, it is possible that there is greater average energy input into the magnetosphere/ionosphere system during far declining phases of the solar cycle compared with those during solar maximum. The discontinuities and magnetic decreases (MDs) associated with interplanetary Alfven waves may be important for geomagnetic activity. In conclusion, it will be shown that geomagnetic storms associated with high-speed streams/CIRs will have the same initial, main, and “recovery” phases as those associated with ICME-related magnetic storms but that the interplanetary causes are considerably different.