  We study the interaction between Venus and the solar wind using a global
three-dimensional self-consistent quasi-neutral hybrid (QNH) model. The model
treats ions (H+, O+) as particles and electrons as a massless charge
neutralising fluid. In the analysed Parker spiral interplanetary magnetic field
(IMF) case (IMF = [8.09, 5.88, 0] nT) a notable north-south asymmetry of the
magnetic field and plasma exists, especially in the properties of escaping
planetary O+ ions. The asymmetry is associated with ion finite gyroradius
effects. Furthermore, the IMF x-component results in a dawn-dusk asymmetry.
Overall, the QNH model is found to reproduce the main observed plasma and
magnetic field regions (the bow shock, the magnetosheath, the magnetic barrier
and the magnetotail), implying the potential of the developed model to study
the Venusian plasma environment and especially the non-thermal ion escape.
