Authors: Daniel Carpenter (University of Michigan), Susan Lepri (University of Michigan), Liang Zhao (University of Michigan)

Continuous studies of the solar wind have been carried out for several decades, seeking to explain how the solar corona is heated, accelerated, and released. The extensive solar wind observations have made the comparison of the solar wind properties across the 11 year solar cycle possible. In this work, we visualize detailed charge state distributions in multiple wind speed regimes to examine how they evolve over the solar cycle. We categorize the in-situ solar wind composition by phase of solar activity, and by wind speed regime. We examine discrete and bimodal binning schemes. We find that there are patterns for the charge states with solar activity which have a general agreement amongst all elements. The fast wind experienced a shift from higher to lower charge states over solar cycle 23; however, the slow wind experienced this as well, albeit coinciding with a depletion of heavy ions in the slow solar wind as a whole. The differences between fast and slow wind were predictably more pronounced in solar minimum than in solar maximum, although trends such as ordering along ionization levels were not as consistent with low FIP elements. We find that the inclusion of more charge states describes finer qualities that may be helpful in constraining models to show how the interplay of electron temperature, plasma density, and wind speed result in a depletion of heavy elements and reduction in ionization levels across Solar Cycle 23.