The dynamics of the Venus ionosphere. I - A simulation of the solar wind compression of the upper dayside ionosphere

Details The dynamics of the Venus ionosphere. I - A simulation of the solar wind compression of the upper dayside ionosphere The dynamics of the Venus ionosphere. I - A simulation of the solar wind compression of the upper dayside ionosphere

Oct 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982jgr....87.8118w&link_type=abstract

Journal of Geophysical Research, vol. 87, Oct. 1, 1982, p. 8118-8130.

Physics

9

Atmospheric Circulation, Atmospheric Density, Compression Waves, Planetary Ionospheres, Solar Activity Effects, Solar Wind, Upper Ionosphere, Venus Atmosphere, Ionospheric Temperature, Pioneer Venus Spacecraft, Shock Wave Interaction, Two Fluid Models

Scientific paper

One of the most exciting discoveries by the Pioneer Venus mission is the extreme variability in the structure of the Venus atmosphere. The solar wind plays a major, although as yet not well-defined, role in the dynamics of the ionosphere. An investigation is being conducted regarding the response of the dayside Venus ionosphere to changing solar wind conditions, in particular to the varying solar wind dynamic pressure. In the present study the dynamics of the upper (h equal to or greater than 200 km) ionosphere are simulated numerically using a one-dimensional, spherically symmetric, Lagrangian hydrodynamic code developed by Stein and Schwartz (1972). The ionosphere is assumed to be unmagnetized and is represented with a two-fluid model. The initial ionosphere is chosen to be in pressure equilibrium with the solar wind at the ionopause. It is shown how some of the time-dependent features of the Venus ionosphere may be simulated with the considered model.

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