The accumulation of interplanetary magnetic fluxes around the Venus ionopause is examined in the light of the PVO magnetometer and plasma wave measurements. It is argued that convective electric currents within the ionosphere are not sufficient to account for the observed geometry of the magnetic profiles. It is suggested that turbulent flow conditions forced in the ionosheath by the interaction process with the ionospheric plasma should produce an anomalous resistivity in the local flow and an effective lag in the transport of the interplanetary magnetic obstacle. The enhanced magnetic fluxes seen above the ionopause should result from effective turbulent currents generated throughout the region of interaction.