Fluvial channels on Titan: Initial Cassini RADAR observations

Cassini radar images show a variety of fluvial channels on Titan’s surface, often several hundreds of kilometers in length. Some
(predominantly at low- and mid-latitude) are radar-bright and braided, resembling desert washes where fines have been removed by
energetic surface liquid flow, presumably from methane rainstorms. Others (predominantly at high latitudes) are radar-dark and
meandering and drain into or connect polar lakes, suggesting slower-moving flow depositing fine-grained sediments. A third type, seen
predominantly at mid- and high latitudes, have radar brightness patterns indicating topographic incision, with valley widths of up to
3 km across and depth of several hundred meters. These observations show that fluvial activity occurs at least occasionally at all latitudes,
not only at the Huygens landing site, and can produce channels much larger in scale than those observed there. The areas in which
channels are prominent so far amount to about 1% of Titan’s surface, of which only a fraction is actually occupied by channels. The
corresponding global sediment volume inferred is not enough to account for the extensive sand seas. Channels observed so far have a
consistent large-scale flow pattern, tending to flow polewards and eastwards.