Physics
Scientific paper
Oct 1990
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990soph..129..387s&link_type=abstract
Solar Physics (ISSN 0038-0938), vol. 129, Oct. 1990, p. 387-405.
Physics
87
Interplanetary Magnetic Fields, Magnetohydrodynamics, Shock Wave Propagation, Solar Wind, Solar Wind Velocity, Spherical Coordinates, Stellar Mass Ejection
Scientific paper
The present parametric study of interplanetary shock propagation to 1 AU uses a two- and-one-half-dimensional MHD time-dependent model whose input conditions encompass initial shock velocity, driving-pulse duration, and pulse width at the near-sun position of 18 solar radii. It is found that, for input pulses with modest angular width and temporal duration, the propagation of the resulting interplanetary fast-forward shock waves primarily depends on the net input energy. While the properties of the reverse shocks are also a function of input energy, they depend on the specific values of the input pulse shock velocity, width, and duration.
Dryer Murray
Smith Zdenka
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