We have used the ion composition data from the CIS/CODIF instrument on Cluster to study ion transport from the cusp to the plasma sheet during storm and non-storm times. The Cluster trajectory, which moves over the polar cap, into the lobe, and then into the plasma sheet on each orbit, allows us to track the changes in O+ in these regions during different levels of activity.  During storms, we find that changes in the O+ density and pressure in the plasma sheet are similar to those commonly observed in the ring current during a storm.  The O+ is low pre-storm.  It increases by about a factor of 10 just prior to or during the early main phase of the storm, and is reduced, but usually not down to pre-storm levels, in the recovery phase. The lobes contain tailward streaming O+ which originates in the Òcleft ion fountain.Ó  During the storm main phase, this population also increases.  A detailed look at the main phase passes shows that a significant increase in the O+/H+ ratio is observed when this lobe population reaches the plasma sheet, and this population becomes incorporated into the plasma sheet, scattering and isotropizing as it crosses the neutral sheet. The inward convection of this population is likely a significant contributor to the storm time ring current.  During non-storm times, the cusp outflow is still observed in the lobes about 13% of the time, and the non-storm times provide better statistics for determining the transport path.  The path of the O+ to the lobe depends strongly on IMF By.  For positive By, the O+ from the Northern cusp flows predominantly to the dawnside, while O+ from the Southern cusp flows to the duskside. For negative IMF By, the transport is much more symmetric. A similar lack of mirror symmetry between positive and negative By has been observed in the convection patterns over the polar cap, and has been shown to result from day/night differences in ionospheric conductivity. Finally we find that the cusp outflow that reaches the ~20 Re plasma sheet is significantly reduced during solar minimum, much more than the outflow itself is reduced, as observed over the cusp and polar cap.  This indicates that during solar minimum, a greater fraction of the O+ escapes down the tail, reducing the ionospheric contribution to the near-earth plasma sheet and ring current.