Volume of Valley Networks on Mars and Its Hydrologic Implications

Abstract:

Valley networks on Mars are river-like features that offer the best evidence for water activities in its geologic past. Previous studies have extracted valley network lines automatically from digital elevation model (DEM) data and manually from remotely sensed images. The volume of material removed by valley networks is an important parameter that could help us infer the amount of water needed to carve the valleys. A progressive black top hat (PBTH) transformation algorithm has been adapted from image processing to extract valley volume and successfully applied to simulated landform and Ma’adim Valles, Mars. However, the volume of valley network excavation on Mars has not been estimated on a global scale. In this study, the PBTH method was applied to the whole Mars to estimate this important parameter. The process was automated with Python in ArcGIS. Polygons delineating the valley associated depressions were generated by using a multi-flow direction growth method, which started with selected high point seeds on a depth grid (essentially an inverted valley) created by PBTH transformation and grew outward following multi-flow direction on the depth grid. Two published versions of valley network lines were integrated to automatically select depression polygons that represent the valleys. Some crater depressions that are connected with valleys and thus selected in the previous step were removed by using information from a crater database. Because of large distortion associated with global dataset in projected maps, the volume of each cell within a valley was calculated using the depth of the cell multiplied by the spherical area of the cell. The volumes of all the valley cells were then summed to produce the estimate of global valley excavation volume. Our initial result of this estimate was ~2.4×10¹⁴ m³. Assuming a sediment density of 2900 kg/m³, a porosity of 0.35, and a sediment load of 1.5 kg/m³, the global volume of water needed to carve the valleys was estimated to be ~7.1×10¹⁷ m³. Because of the coarse resolution of MOLA data, this is a conservative lower bound. Comparing with the hypothesized northern ocean volume 2.3×10¹⁶ m³ estimated by Carr and Head (2003), our estimate of water volume suggests and confirms an active hydrologic cycle for early Mars. Further hydrologic analysis will improve the estimate accuracy.