Comets are among the most primitive bodies in the solar system that typify the remnant materials from which all the larger planets and moons were constructed. Consequently, they are like "time capsules", allowing us to glimpse into the initial conditions of our Solar System. However, geologic processes have been shown to alter the surfaces of comets (especially Jupiter Family Comets) as they make their journeys through the inner solar system. Hence, to accurately leverage what comets may tell us about our origins, we must first understand how these active geological process have shaped and altered their primitive surfaces. One of the primary landscapes observed on all comets to date are smooth terrains – large sedimentary basins that serve as the terminal sink for airfalling sediment. Owing to their insulating nature and vast spatial extents, cometary smooth terrains credibly govern the general level and behavior of cometary activity observable from ground-based telescopes and the long-term thermal evolution of cometary interiors, helping preserve any remnant primitive materials. Thought to be largely ice-depleted granular lag deposits, Rosetta instead showed that the vast majority of changes on comet 67P took place within its smooth terrains. Such unexpected changes therefore challenge our basic understanding of how comets erode, and how they may be used as windows into the earliest portions of the Solar System. Herein, we present a study of the surface activity and sediment re-distribution mechanisms within comet 67P's smooth terrains. In Chapter 2, we demonstrate that the time and location of the onset of erosion driven by scarp-retreat is controlled by local topography rather than surface inhomogeneities in volatile content. In Chapters 3 and 4, we provide measurements of sediment re-distribution within 67P's smooth terrains, highlighting that local-scale processes dominate over 67P's seasonally driven dust transport in the overall re-distribution of sediment. Additionally, in Chapter 4, we also discuss a dust transport model to calculate sediment transport pathways across 67P's nucleus, allowing us to determine where sediment may be transported to/from. Finally, in Chapter 5, we demonstrate that similar surface morphologies may exist across the surfaces of all resolved JFCs, indicating that they follow similar evolutionary pathways where any differences in their bulk appearance is a direct result of the amount of time they have spent in the inner solar system.