The Super Dual Auroral Radar Network (SuperDARN) is a collection of radars built to study ionospheric convection. We use a 7‐year archive of SuperDARN convection maps, processed in 3 different ways, to build a statistical understanding of dusk‐dawn asymmetries in the convection patterns. We find that the data set processing alone can introduce a bias which manifests itself in dusk‐dawn asymmetries. We find that the solar wind clock angle affects the balance in the strength of the convection cells. We further find that the location of the positive potential foci is most likely observed at latitudes of 78° for long periods (>300 min) of southward interplanetary magnetic field (IMF), as opposed to 74° for short periods (<20 min) of steady IMF. For long steady dawnward IMF the median is also at 78°. For long steady periods of duskward IMF, the positive potential foci tends to be at lower latitudes than the negative potential and vice versa during dawnward IMF. For long periods of steady Northward IMF, the positive and negative cells can swap sides in the convection pattern. We find that they move from ∼0–9 MLT to 15 MLT or ∼15–23 MLT to 10 MLT, which reduces asymmetry in the average convection cell locations for Northward IMF. We also investigate the width of the region in which the convection returns to the dayside, the return flow width. Asymmetries in this are not obvious, until we select by solar wind conditions, when the return flow region is widest for the negative convection cell during Southward IMF. Plain Language Summary At high latitudes, near the Earth's magnetic pole, the ionosphere moves around in a dual‐cell pattern: The convection moves from the dayside, over the magnetic pole toward the nightside and then flows return back to the dayside at lower latitudes. Both cells tend to be centered away from the pole, one toward the dusk side and one toward the dawn side. The two cells have a tendency to be asymmetric with the dusk cell typically larger and stronger. Asymmetries in the two convection cells are often attributed to changes in the solar wind as there is a physical connection between the ionosphere and the solar wind. The mechanisms which describe this interaction are well known but some of the data sets with which we measure ionospheric convection have unquantified uncertainties associated with them. One of the longest running measurement systems of the ionospheric convection is the Super Dual Auroral Radar Network (SuperDARN). This ground‐based system was built specifically to measure ionospheric convection and it is often used to make convection maps of the ionosphere. Over the years, more radars have been added to the network and the software used to process the data has been updated. In this study we use different versions of the convection maps to statistically investigate 7 years of ionospheric convection asymmetries and understand which of the asymmetries were introduced by a change in the data set and which by the solar wind. We look at the location and strength of the cells and the width of the return flow region, which constrains the size of the cells. Key Points We study dusk‐dawn asymmetries in 7 years of Super Dual Auroral Radar Network convection maps which are introduced by solar wind orientations, or data processing Asymmetries due to interplanetary magnetic field By can occur in the strength and location of the convection cells, and the return flow width Asymmetries due to the background model are likely to occur in the locations of the convection cells