Estimation of the erosion rate of Venus ionosphere due to viscous like interaction with the solar wind

Details Estimation of the erosion rate of Venus ionosphere due to viscous like interaction with the solar wind Estimation of the erosion rate of Venus ionosphere due to viscous like interaction with the solar wind

Dec 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009agufm.p11b1201r&link_type=abstract

American Geophysical Union, Fall Meeting 2009, abstract #P11B-1201

Physics

Plasma Physics

[2459] Ionosphere / Planetary Ionospheres, [5435] Planetary Sciences: Solid Surface Planets / Ionospheres, [6295] Planetary Sciences: Solar System Objects / Venus, [7859] Space Plasma Physics / Transport Processes

Scientific paper

On the basis of the results of 2D, multispecies numerical simulations of the viscous-like interaction of the solar wind with the upper ionosphere of Venus, we review previous estimations of Perez-de-Tejada (2004,2006) of the rate of removal of ionospheric material by the solar wind. As numerical simulations indicate, after a significant change in the IMF direction, when the erosion of a new portion of the ionosphere by viscous-like forces begins, there is an episode of strong erosion as ionospheric channels are "carved out". Depending on the incident solar wind density and velocity, the mass removal rate from the upper ionosphere during this period can be significantly greater than previously estimated values. We estimate an average value of the mass removal rate from the ionosphere of Venus in terms of a particular model for the variability of the IMF and the solar wind conditions and compare it to estimations on the basis of Venus Express observations.

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