A new computational model for the prediction of mass loading phenomena for solar wind interactions with cometary and planetary ionospheres

Details A new computational model for the prediction of mass loading phenomena for solar wind interactions with cometary and planetary ionospheres A new computational model for the prediction of mass loading phenomena for solar wind interactions with cometary and planetary ionospheres

Jun 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987aiaa.conft....s&link_type=abstract

AIAA, Fluid Dynamics, Plasma Dynamics, and Lasers Conference, 19th, Honolulu, HI, June 8-10, 1987. 12 p.

Physics

Fluid Dynamics

Cometary Atmospheres, Gas Dynamics, Magnetic Fields, Planetary Ionospheres, Plasma Interactions, Solar Wind, Conservation Equations, Continuity Equation, Mathematical Models, Rankine-Hugoniot Relation, Shock Waves, Venus (Planet)

Scientific paper

The modified gasdynamic convected-magnetic-field MHD model developed by Spreiter and Stahara (1980) to simulate the supersonic flow of the solar wind past planetary magnetoionospheres is extended to account for cases (such as Venus and comets) in which significant numbers of neutral atmospheric atoms become ionized in the surrounding flow and add to its momentum, energy, and mass. The mathematical model and the solution procedures for the nose and tail regions are explained; typical computational grids are shown; and numerical results for a comet and for the Venus ionosheath and bow shock are presented graphically. It is found that the bow shock weakens and moves further upstream of the obstacle as mass loading is increased and the flow upstream of the bow shock becomes more compressed.

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