Convective studies involving ion flow in the Venus dayside ionosphere are used to understand the nature of the observed O\sb2\sp+ distribution. Flows are modeled (not calculated) from previous data and theory which are incorporated to determine the ion distributions for O\sp+, CO\sb2\sp+, and O\sb2\sp+. Current understanding of ion chemistry and related parameters are used in solving the continuity equation in two dimensions to provide ion profiles at different solar zenith angles. To explain the O\sb2\sp+ distribution, downward flow with speeds of approximately 500 m/s are required.