MHD simulation of an interaction of a shock wave with a magnetic cloud
MHD simulation of an interaction of a shock wave with a magnetic cloud
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DOI：
10.1029/97ja01675
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发表时间：
1997-10
影响因子：
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通讯作者：
M. Vandas;S. Fischer;M. Dryer;Z. Smith;T. Detman;A. Geranios
中科院分区：
文献类型：
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作者：
M. Vandas;S. Fischer;M. Dryer;Z. Smith;T. Detman;A. Geranios
行星际冲击波在日光层中的传播速度比早期发射的日冕喷出物快，在这种相互作用期间穿透它们并修改它们的参数。使用二维和一维半MHD模拟，我们展示了如何磁云（通量绳）传播的速度比周围的太阳风的3倍，是由一个更快的旅行冲击波超越云的影响。在相互作用期间，云内部的磁场增加，因为它在径向方向上被压缩并变得非常扁。云也被加速，移动得更快，作为一个整体，而两个冲击（由云和更快的行星际冲击驱动）在云的上游合并。这种相互作用可能是一种相当普遍的现象，因为在太阳活动活跃的时期，日冕物质抛射和冲击波的发生频率很高。
Interplanetary shock waves, propagating in the heliosphere faster than earlier-emitted coronal ejecta, penetrate them and modify their parameters during this interaction. Using two and one half dimensional MHD simulations, we show how a magnetic cloud (flux rope) propagating with a speed 3 times higher than the ambient solar wind is affected by an even faster traveling shock wave overtaking the cloud. The magnetic field increases inside the cloud during the interaction as it is compressed in the radial direction and becomes very oblate. The cloud is also accelerated and moves faster, as a whole, while both shocks (driven by the cloud and the faster interplanetary shock) merge upstream of the cloud. This interaction may be a rather common phenomenon due to the frequency of coronal mass ejections and occurrence of shock waves during periods of high solar activity.