Motion of shocks through interplanetary streams

Details Motion of shocks through interplanetary streams Motion of shocks through interplanetary streams

Oct 1975

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975jgr....80.4004b&link_type=abstract

Journal of Geophysical Research, vol. 80, Oct. 1, 1975, p. 4004-4010.

Astronomy and Astrophysics

Astronomy

1

Gas Dynamics, Interplanetary Medium, Shock Wave Interaction, Solar Wind, Astronomical Models, Mach Number, Magnetohydrodynamic Flow, Shock Fronts, Solar Flares

Scientific paper

A model for the motion of flare-generated shocks through interplanetary streams is presented which illustrates the effects of a stream-shock interaction on the shock strength and geometry. It is a gasdynamic calculation based on Whitham's (1958) method and on an empirical approximation for the relevant characteristics of streams. The results show that the Mach number of a shock can decrease appreciably to near unity in the interaction region ahead of streams and that the interaction of a spherically symmetric shock with a spiral-shaped corotating stream can cause significant distortions of the initial shock-front geometry. The geometry of a shock discussed by Lepping and Chao (1972) is qualitatively explained by this model.

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