3-D simulation of high-latitude interaction regions: Comparison with ULYSSES results

Details 3-D simulation of high-latitude interaction regions: Comparison with ULYSSES results 3-D simulation of high-latitude interaction regions: Comparison with ULYSSES results

Sep 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994georl..21.2063p&link_type=abstract

Geophysical Research Letters (ISSN 0094-8276), vol. 21, no. 18, p. 2063-2066

Statistics

Computation

43

Magnetohydrodynamics, Solar Corona, Solar Planetary Interactions, Solar Wind, Three Dimensional Models, Computational Grids, Computerized Simulation, Magnetic Flux, Shock Waves, Three Dimensional Flow, Ulysses Mission

Scientific paper

A three-dimensional (3-D) magnetohydrodynamic (MHD) numerical model is used to simulate the global evolution of a steady, tilted-dipole solar wind flow configuration similar to that prevalent in interplanetary space in 1993. Systematic latitudinal changes in the structure of a corotating interaction region (CIR) near 5 AU is shown to agree well with recent Ulysses observations. The abrupt disappearance of forward shocks and continued persistence of reverse shocks poleward of the latitude where Ulysses crossed the southern edge of the coronal streamer belt is explained as a natural consequence of the 3-D flow geometry.

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