Abstract
The adiabatic motion of a hydromagnetic fluid behind a strong spherical fast shock wave is examined in the case when the ambient medium exactly follows prescriptions of Parker's solar wind model for the far field and when the shock propagation is at a uniform velocity. In the analysis, both the spiralling Archimedian magnetic field and the wind streaming of the interplanetary medium are considered. It is found that the magnetic field controls the wave details at the rear termination where both the density and the magnetic field reach peak values, and that 3 2 for the polytrope index represents a critical value dividing waves having divergent characterizations at the termination. The active kinking distortion of interplanetary flux lines by the flare-induced blastwave is considered. Representative waves corresponding to a 1200 km/sec-velocity shock wave are calculated and presented for demonstration.
Published Version
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