Venus’s thick atmosphere rotates in the same direction as the solid body, but ~60 times faster. This atmospheric superrotation has produced dozens of windblown ejecta deposits (“parabolas”) on the surface of Venus. The formation and modification of parabolas is an interplay between impacts, aeolian erosion, and atmospheric dynamics. We conducted a survey to explore the nature of these sedimentary surface features and obtained three new results. Firstly, we observe trends in parabolas’ morphology that shed light on how they are deposited and eroded. Changes in the size and radar albedo of parabolas are likely linked to the height and density (respectively) of ejecta plumes at time of formation. Next, we discovered that parabolas show orientations inconsistent with present atmospheric dynamics, and thus may record a change in these dynamics or geologically recent true polar wander at a rate of ~1° Myr-1. Lastly, we observe a definitive example of a volcanically embayed parabola, which provides strong evidence for large-scale geologic activity in the recent past. These results provide important insights into the history and character of geologic processes on Venus that will guide observations by upcoming missions. If true polar wander is the cause of the anomalous parabola orientations, then atmospheric superrotation has probably persisted for at least the age of Venus’s surface. This mode of atmospheric circulation is unique to Venus in the inner Solar System, but is likely common to terrestrial exoplanets that are tidally locked in close orbits to their parent stars.