Numerical solution of the steady-state solar wind

Details Numerical solution of the steady-state solar wind Numerical solution of the steady-state solar wind

Sep 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984baicz..35..317o&link_type=abstract

Astronomical Institutes of Czechoslovakia, Bulletin (ISSN 0004-6248), vol. 35, no. 6, 1984, p. 317-326.

Statistics

Computation

3

Computational Astrophysics, Computational Fluid Dynamics, Solar Wind, Computer Programs, Hydrodynamics, Ideal Fluids, Inviscid Flow, Mach Number, Shock Wave Propagation, Steady State

Scientific paper

The one-dimensional time-dependent hydrodynamic computer code BOREAS (Odstrcil, 1984) is applied to the solution of the steady-state solar wind. The relaxation technique is used; i.e., starting from an arbitrary state the final steady state is obtained. However, this process is more complex than relaxation alone. In particular, the reverse shock is formed at the inner boundary, and near this extreme shock strong numerical oscillations are observed. A detailed analysis of this process is given together with results obtained under different conditions. The solution presented may be used directly for an interplanetary-shock-wave simulation.

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