Numerical Simulation of the Formation of Venus Ionospheric Channels due to Viscous Dragging by the Solar Wind

Details Numerical Simulation of the Formation of Venus Ionospheric Channels due to Viscous Dragging by the Solar Wind Numerical Simulation of the Formation of Venus Ionospheric Channels due to Viscous Dragging by the Solar Wind

Dec 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agufm.p13b1313r&link_type=abstract

American Geophysical Union, Fall Meeting 2008, abstract #P13B-1313

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5435 Ionospheres (2459), 6295 Venus, 7859 Transport Processes

Scientific paper

We present results of the numerical simulation of the process of formation of ionospheric channels in Venus as a consequence of the viscous interaction of the solar wind with ionospheric gas. A 2D, hydrodynamical, two species, computational code has been developed to solve the Navier-Stokes, continuity and energy equations allowing us to study simultaneously the dynamics of the solar wind flow and material in the upper layers of the ionosphere. The results of our simulations depend mainly on the value of the 3 adimensional parameters of the problem: the Mach number of the incident solar wind, the effective Reynolds number of the shocked solar wind and ionospheric material and the ratio of the timescale for interspecies coupling to the crossing time for the shocked solar wind. On the basis of our results we estimate that the timescale for channel formation is typically of the order of tens of minutes. Complementing our 2D results with analytical calculations we can also estimate the amount of mass removed from the ionosphere of the planet as a function of time and the shape of the resulting ionospheric channels, although these features are more strongly dependent on the parameters of the simulation. Finally, we compare our results to the known properties of ionospheric channels as derived from the in situ measurements in the ionosphere of Venus.

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