Abstract
Observations of flare associated shock waves have led to a better understanding of the general features occurring during the interaction between the fast ejected gas and the slow ambient plasma. A description of the different regions observed in shock waves is briefly presented as well as the characteristics of the discontinuities between them. The configuration of these waves as they expand through the interplanetary medium is discussed from multi-spacecraft data as well as from IPS observations, and the results are compared with the shape and behavior predicted by theoretical models. The evolution of the characteristics of the interplanetary medium is rather well explained through MHD time-dependent computations, and the non-spherical shape of the waves is well reproduced by two dimensional models. However, several features differ from the simulated evolution. These discrepancies are attributed either to the lack of theoretical refinements (e.g., heat conduction, multifluid coupling) or to inhomogeneities in the interplanetary medium.
Published Version
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