Study of the formation, evolution, and decay of shocks in the heliosphere between 0.5 and 30.0 AU

Details Study of the formation, evolution, and decay of shocks in the heliosphere between 0.5 and 30.0 AU Study of the formation, evolution, and decay of shocks in the heliosphere between 0.5 and 30.0 AU

Jan 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985jgr....90..217s&link_type=abstract

Journal of Geophysical Research (ISSN 0148-0227), vol. 90, Jan. 1, 1985, p. 217-220.

Physics

18

Heliosphere, Magnetohydrodynamics, Shock Fronts, Solar Wind, Radial Velocity, Shock Wave Attenuation, Temporal Distribution, Temporal Resolution

Scientific paper

The spatial and temporal evolution of corotating interaction regions is examined between 0.5 and 30 AU using a solar wind simulation with a continuous sinusoidally varying velocity, density, and temperature input pulse train. The authors show (1) the well-known formation of forward-reverse MHD shock ensembles, followed by (2) their interaction that results in a highly nonlinear "pressure" wave that eventually reforms into a new but more irregular set of forward-reverse shock pairs. As a result of these compound interactions, the overall temperature decays much more slowly than the classical steady state adiabatic radial dependency of R-4/3.

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