Geomorphic Analysis of North Polar Channel Networks on Titan, and Implications for Active Tectonics and Persistence of Relief Structures

Details Geomorphic Analysis of North Polar Channel Networks on Titan, and Implications for Active Tectonics and Persistence of Relief Structures Geomorphic Analysis of North Polar Channel Networks on Titan, and Implications for Active Tectonics and Persistence of Relief Structures

Dec 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009agufm.p51c1138c&link_type=abstract

American Geophysical Union, Fall Meeting 2009, abstract #P51C-1138

Mathematics

Logic

[5415] Planetary Sciences: Solid Surface Planets / Erosion And Weathering, [5419] Planetary Sciences: Solid Surface Planets / Hydrology And Fluvial Processes

Scientific paper

Investigation of SAR-mode imagery, gathered by the Cassini orbiter’s RADAR instrument, suggests that channel networks are a common surface feature on Saturn’s moon of Titan. Around the north pole of Titan, channel networks drain into large radar dark spots previously interpreted as large lakes and seas filled with liquid hydrocarbons (located above 70°N and between 210°W and 300°W). We selected three north polar channel networks on Titan (referred to herein as Basin A, Basin B, and Basin C) for morphometric analysis, giving bifurcation ratios of 2.6, 8.1, and 3.4, respectively; two Terrestrial analog basins located in arid and tectonically-active regions produced network bifurcation ratios of 3.4 and 5.5 (coastal Oman and central Nevada, respectively). Stream ordering analysis shows that the Titan networks contain between 2 - 4 orders of visible channel segments (limited by the imager resolution); comparable imagery of the Terrestrial basins indicates that between 3 and 5 stream orders are discernible. Analysis of the sediment transport potential in Titan’s Basin A suggests that the critical flow depths required to entrain water-ice grains with a 75 mm diameter range from 1.0 m - 1.5 m (depending on local slope). Assuming constant 1.5 m depth liquid hydrocarbon flow during the summer (wet) season, we estimated that roughly 19,800 Titan years are required to lower Basin A down to its minimum relief. The developing topographic picture [Stiles et al., 2009] of the north polar ‘Lake District’ on Titan, coupled with the morphological similarities shared by the channel networks on Titan and drainage basins in tectonically active regions of Earth, suggests that recent tectonic uplift could help explain why this region displays variable relief, as well as contorted and constricted channel networks. Additional controls on drainage network morphology may include climatically-driven, seasonal base-level fluctuations of the liquid hydrocarbon maria.

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