Induced Magnetospheric Features Due to the Obrital Motion of Venus

Lundin et al., [2012] analyzed ion data from 390 Venus Express (VEX) orbits and found several asymmetric features most pronounced near the Poles and in the tail/nightside region. They hypothesized that these features were due to the planets orbital motion about the Sun. Lundin et al., [2012] further postulated that the orbital motion of the planet leads to a asymmetric influx of solar wind ions that drives the super rotation of the upper atmosphere. The hypotheses of Lundin et al., is tested using global hybrid simulations of the Venus solar wind interaction that ignore and include the orbital motion of the planet. We compare the changes in the magnetospheric structures surrounding Venus due to the orbital effects. The ion energy and momentum deposition rates into the neutral atmosphere are examined. The plausibility that the ion deposition drives the super rotation of the upper Venusian atmosphere is discussed.