Astronomy and Astrophysics – Astronomy
Scientific paper
Jul 1993
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993pdl..confq....h&link_type=abstract
AIAA, Plasmadynamics and Lasers Conference, 24th, Orlando, FL, July 6-9, 1993, 11 p.
Astronomy and Astrophysics
Astronomy
Algorithms, Computerized Simulation, Interplanetary Magnetic Fields, Magnetohydrodynamic Waves, Solar Wind, Boundary Conditions, Iteration, Shock Wave Propagation, Time Marching
Scientific paper
In the present study, transient, 1-dimensional, 3-vector component MHD equations are used to simulate steady and unsteady, thermally conductive MHD solar wind expansions between the solar surface and 1 AU (astronomical unit). A variant of SIMPLE numerical method was used to integrate the equations. Steady state solar wind properties exhibit qualitatively similar behavior with the known Weber-Davies Solutions. Generation of Alfven shock, in addition to the slow and fast MHD shocks, was attempted by the boundary perturbations at the solar surface. Property changes through the disturbance were positively correlated with the fast and slow MHD shocks. Alfven shock was, however, not present in the present simulations.
Dryer Murray
Han Shensheng
Wu Shi Tsan
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