The forward-reverse shock pair at large heliocentric distances

Details The forward-reverse shock pair at large heliocentric distances The forward-reverse shock pair at large heliocentric distances

Sep 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984jgr....89.7367w&link_type=abstract

Journal of Geophysical Research (ISSN 0148-0227), vol. 89, Sept. 1, 1984, p. 7367-7379.

Astronomy and Astrophysics

Astronomy

37

Interplanetary Medium, Magnetohydrodynamics, Shock Wave Interaction, Solar Wind, Astronomical Models, Convergence, Propagation Modes, Propagation Velocity, Rarefaction, Unsteady State, Velocity Distribution

Scientific paper

An unsteady one-dimensional numerical magnetohydrodynamic (MHD) model is developed in order to study the essential physical processes involved in the development of the forward-reverse shock pair in the heliosphere. In the model, MHD shocks are treated as boundary surfaces which divide the domain of interest in the r-t plane into several flow regions. The positions of the shock boundary surfaces between two neighboring flow regions are determined by shock speed. On the basis of integrations of the model, it is found that the strong MHD disturbances generated in a corotating interaction region (CIR) propagate at a fast speed relative to the moving material, and that the wave propagation speed is greater in CIR than in its surroundings. This causes disturbances in CIR to pile up and form a shock pair. The newly formed shock pair will in turn propagate outward from the leading edge to interact with ambient rarefaction regions. This interaction accounts for the double sawtooth configuration observed in velocity profiles of shock pairs. It is also demonstrated that the merging of two shocks produces a stronger shock and constant surface on its backside. Computer generated velocity profiles based on the model are presented.

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