Forward-reverse Shock Pairs Associated with Coronal Mass Ejections
نویسنده
چکیده
For some coronal mass ejections (CMEs), their interaction with the ambient solar wind can produce a forward-reverse shock pair. The high-speed mass ejecta compresses the plasma near the top of the CME on both sides of the tangential discontinuity which separates the CME plasma from the ambient solar wind plasma. The front of the compressed CME plasma propagates in the reverse direction relative to the ejecta flow, it may steepen to from a reverse slow shock. The front of the compressed solar wind plasma also propagates in the forward direction relative to the ambient solar wind and it may steepen to form a forward shock. The forwardreverse shock pair associated with CMEs moves outward in interplanetary space and evolves into a pair of fast shocks. The interplanetary manifestation of some CMEs is pictured as a magnetic cloud accompanied by a shock pair: a forward shock precedes the cloud and a reverse shock either within or behind the cloud.
منابع مشابه
Reply to comment by P. Riley and J. T. Gosling on ‘‘Are high-latitude forward-reverse shock pairs driven by overexpansion?’’
[1] During its passage through the high-latitude heliosphere, Ulysses observed interplanetary coronal mass ejections (ICMEs) bounded by forward-reverse shock pairs. Gosling et al. [1995] originally proposed the shock pairs form as a result of CME overexpansion into the ambient solar wind. Manchester and Zurbuchen [2006] suggested an alternative explanation for forward-reverse shock pairs in whi...
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