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Mars' surface bears the imprint of valley networks formed billions of yearsago and their relicts can still be observed today. However, whether thesenetworks were formed by groundwater sapping, ice melt, or fluvial runoff hasbeen continuously debated. These different scenarios have profoundly differentimplications for Mars' climatic history, and thus for its habitability in thedistant past. Recent studies on Earth revealed that channel networks in aridlandscapes with more surface runoff branch at narrower angles, while in humidenvironments with more groundwater flow, branching angles are much wider. Wefind that valley networks on Mars generally tend to branch at narrow anglessimilar to those found in arid landscapes on Earth. This result supports theinference that Mars once had an active hydrologic cycle and that Mars' valleynetworks were formed primarily by overland flow erosion with groundwaterseepage playing only a minor role.

The role of surface water in the geometry of Mars' valley networks and its climatic implications