Patterns and processes of drainage network evolution on Mars

Large, complex drainage networks exist on the surface of Mars. These drainage patterns suggest that base level change, fluvial erosion, and deposition of sedimentary rock have played important roles in determining the shape of Martian topography. On Earth, base-level change plays the most important role in determining shapes of river profiles at wavelengths greater than a few kilometers. Wavelet transforms of Martian drainage patterns indicate that the same is true for most Martian drainage. For example, rivers in the Warrego Valles system have large convex-upward elevation profiles, with broad knickzones spanning more than 100 kilometers in length and few kilometers in height. More than 90% of the spectra power of rivers in this system resides at wavelengths greater than 10 kilometers. We examine the source of this long wavelength spectra power by jointly inverting suites of Martian river profiles for damped spatio-temporal histories of base-level change. Drainage networks were extracted from the High Resolution Stereo Camera (HRSC) topographic dataset using flow-routing algorithms. Calculated uplift rate histories indicate that regional uplift at wavelengths greater than 100 kilometers play an important role in determining the history of landscape evolution in Warrego Valles. In other regions (e.g. Holden and Eberswalde craters) joint inversion of families of rivers draining craters helps to constrain values of erosional parameters in a simplified version of the stream power erosional model. Integration of calculated incision rates suggest that we can perform a simple mass balance between eroded and deposited rock in regions where both depositional and erosional landforms exist.