Simulation of period doubling of recurrent solar wind structures

Details Simulation of period doubling of recurrent solar wind structures Simulation of period doubling of recurrent solar wind structures

Dec 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990jgr....9520663w&link_type=abstract

Journal of Geophysical Research (ISSN 0148-0227), vol. 95, Dec. 1, 1990, p. 20663-20671.

Physics

11

Period Doubling, Pioneer Space Probes, Solar Rotation, Solar Wind, Computerized Simulation, Coronal Holes, Magnetohydrodynamic Flow, Shock Wave Interaction, Solar Planetary Interactions

Scientific paper

Based on satellite observations of a recurrent solar wind structure conducted in 1974, an MHD simulation model, and input functions generated from plasma and magnetic field data, the continuing evolution of the solar wind structure outside 5 AU is studied. The model uses the Rankine-Hugoniot relations to describe the jumps in flow properties across the shocks, and it treats shocks as surfaces of discontinuity with zero thickness. Two interaction processes (the collision and the merging of shocks) play important roles in restructuring the solar wind in the outer heliosphere. The simulation result shows that period doubling occurs between 5 and 10 AU. The recurrent solar wind appears to be a persistent new structure between 10 and 20 AU, and it consists of one merged interaction region per solar rotation.

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