Hybrid simulations of the O+ ion escape from Venus: Influence of the solar wind density and the IMF x component

Details Hybrid simulations of the O+ ion escape from Venus: Influence of the solar wind density and the IMF x component Hybrid simulations of the O+ ion escape from Venus: Influence of the solar wind density and the IMF x component

May 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009adspr..43.1436l&link_type=abstract

Advances in Space Research, Volume 43, Issue 9, p. 1436-1441.

Computer Science

3

Scientific paper

As an initial effort to study the evolution of the Venus atmosphere, the influence of the solar wind density and the interplanetary magnetic field (IMF) x component (the x-axis points from Venus towards the Sun) on the O+ ion escape rate from Venus is investigated using a three-dimensional quasi-neutral hybrid (HYB-Venus) model. The HYB-Venus model is first applied to a case of the high-density (100 cm-3) solar wind interaction with Venus selected from the Pioneer Venus Orbiter observations to demonstrate its capability for the study. Two sets of simulations with a wide range of solar wind densities and different IMF x components are then performed. It is found that the O+ ion escape rate increases with increasing solar wind density. The O+ ion escape rate saturates when the solar wind density becomes high (above 100 cm-3). The results also suggest that the IMF x component enhances the O+ ion escape rate, given a fixed IMF component perpendicular to the x-axis. Finally, the results imply a higher ion loss rate for early-Venus, when solar conditions were dramatically different.

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