Turbulent processes of mass-loading of new ions on Venus and Mars and the problems of numerical models of the interaction of solar wind with these planets. 1: Characteristics of the flow of solar wind around the planets

Details Turbulent processes of mass-loading of new ions on Venus and Mars and the problems of numerical models of the interaction of solar wind with these planets. 1: Characteristics of the flow of solar wind around the planets Turbulent processes of mass-loading of new ions on Venus and Mars and the problems of numerical models of the interaction of solar wind with these planets. 1: Characteristics of the flow of solar wind around the planets

Apr 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991rpsct...6...40b&link_type=abstract

In its JPRS Report: Science and Technology. USSR: Space p 40 (SEE N91-26162 18-12) Transl. into ENGLISH from Kosmicheskiye Issle

Mathematics

Friction, Heavy Ions, Hydrodynamics, Ionopause, Ions, Mathematical Models, Solar Activity Effects, Solar Position, Solar Wind, Turbulence, Two Fluid Models, Distance, Mars (Planet), Planets, Solar System, Venus (Planet), Zenith

Scientific paper

Initially thought to be due only to solar wind/comet interactions, loading of the solar wind with heavy ions has been found to be the result also of interactions with planets. Is is a universal phenomenon near nonmagnetic and slightly magnetic solar system objects. An overview of previous investigations is given. On Venus, loading is most intense in the transition region near the ionopause. The ions are rapidly accelerated in laminar and turbulent fields. The conditions for the capture of new heavy ions by the solar wind vary substantially with distance from the planet surface and the solar zenith angle. It is impossible to determine the pressure of heavy ions for hydrodynamic calculations without kinetic calculations. Hydrodynamic models developed at solar minimum were found to be inadequate at solar maximum. A two-fluid model with anomalous friction between species of ions is used to described the flow of the solar wind around Venus and Mars. The friction is due to turbulent acceleration processes in the transition region.

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