Alluvial Fans on Titan Reveal Atmosphere and Surface Interactions and Material Transport

Jani Radebaugh 1 Dario Ventra 2 Ralph Lorenz 3 Tom Farr 4 Randolph Kirk 5 Alexander Hayes 6 Michael Malaska 4 Sam Birch 6 Zac Yung-Chun Liu 7 Jonathan Lunine 6 Jason Barnes 8 Alice Le Gall 9, 10 Rosaly Lopes 4 Ellen Stofan 11 Stephen Wall 4 Philippe Paillou 12
LATMOS - Laboratoire Atmosphères, Milieux, Observations Spatiales
LATMOS - Laboratoire Atmosphères, Milieux, Observations Spatiales
12 ASP 2015
L3AB - Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux, OASU - Observatoire aquitain des sciences de l'univers, LAB - Laboratoire d'Astrophysique de Bordeaux [Pessac], UB - Université de Bordeaux
Abstract : Alluvial fans, important depositional systems that record how sediment is stored and moved on planetary surfaces, are found on the surface of Titan, a body of significantly different materials and process rates than Earth. As seen by Cassini’s Synthetic Aperture Radar (SAR) images at 350 m resolution, fans on Titan are found globally and are variable in size, shape and relationship to adjacent landforms. Their morphologies and SAR characteristics, which reveal roughness, textural patterns and other material properties, show similarities with fans in Death Valley seen by SAR and indicate there are regions of high relative relief locally, in the Ganesa, Xanadu and equatorial mountain belt regions. The Leilah Fluctus fans near Ganesa are ~30 km x 15 km, similar to the largest Death Valley fans, and revealing mountainous topography adjacent to plains. Others have gentle slopes over hundreds of kilometers, as in the high southern latitude lakes regions or the Mezzoramia southern midlatitudes, where a fan system is 200 km x 150 km, similar to the Qarn Alam fan emerging into the Rub al Khali in Oman. Additionally, there is evidence for a range of particle sizes, from relatively coarse (~2 cm or more) to fine, revealing long-term duration and variability in erosion by methane rainfall and transport. Some features have morphologies consistent with proximality to high-relief source areas and highly ephemeral runoff, while others appear to draw larger catchment areas and are perhaps characterized by more prolonged episodes of flow. The presence of many fans indicates the longevity of rainfall and erosion in Titan’s surface processes and reveals that sediment transport and the precipitation that drives it are strongly episodic. Alluvial fans join rivers, lakes, eroded mountains, sand dunes and dissolution features in the list of surface morphologies derived from atmospheric and fluvial processes similar to those on Earth, strengthening comparisons between the two planetary bodies.
Type de document :
Communication dans un congrès
AGU Fall Meeting 2015, Dec 2015, San Francisco, United States. pp.P12B-01
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Contributeur : Catherine Cardon <>
Soumis le : mardi 29 décembre 2015 - 17:54:50
Dernière modification le : jeudi 8 juin 2017 - 14:46:29


  • HAL Id : insu-01248994, version 1



Jani Radebaugh, Dario Ventra, Ralph Lorenz, Tom Farr, Randolph Kirk, et al.. Alluvial Fans on Titan Reveal Atmosphere and Surface Interactions and Material Transport. AGU Fall Meeting 2015, Dec 2015, San Francisco, United States. pp.P12B-01. <insu-01248994>



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