We investigated the geologic history of Titan through mapping and analyzing the distribution of observed geomorphic features using a combination of Cassini data collected by RADAR, VIMS, and ISS. Determining the spatial and superposition relations between geomorphologic units on Titan leads to an understanding of the likely time evolution of the landscape and gives insight into the process interactions that drive its evolution. We have used all available datasets to extend the mapping initially done by Lopes et al. . We now have a global map of Titan at 1:800,000 scale in all areas covered by Synthetic Aperture Radar (SAR). We have defined six broad classes of terrains following Malaska et al. , largely based on prior mapping . These broad classes are: craters, hummocky/mountainous, labyrinth, plains, lakes, and dunes. We have found that the hummocky/mountainous terrains are the oldest units on the surface and appear radiometrically cold, indicating icy materials . Dunes are the youngest units and appear radiometrically warm, indicating organic sediments. VIMS analysis shows that compositional variations can also exist within the same class of unit [4, 5]. Using correlations between different data sets, we have extended the map to regions not covered by SAR to produce a global 1:2,000,000 scale map. References:  Lopes, R.M.C., et al.: Icarus, 205, 540-588, 2010;  Malaska, M., et al., Icarus, 270, 130-161, 2016;  Janssen et al., 2016 Icarus 270, 443-459, 2016.  Solomonidou, A., et al.: Icarus 270, 85-99, 2016,  Lopes, R.M.C., et al, Icarus, 270, 162-182, 2016.
AAS/Division for Planetary Sciences Meeting Abstracts #50
- Pub Date:
- October 2018