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Publication Details
AFRICAN RESEARCH NEXUS
SHINING A SPOTLIGHT ON AFRICAN RESEARCH
earth and planetary sciences
Morphological and mechanical characterization of gullies in a periglacial environment: The case of the Russell crater dune (Mars)
Planetary and Space Science, Volume 71, No. 1, Year 2012
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Description
Gullies on terrestrial sand dunes are rare, and their presence on Mars, as well as their mechanical properties, and the quantity of fluid required for their formations currently remain poorly understood. This study focuses on gully morphologies on the Russell megadune (54.5°S; 12.7°E) using High Resolution Imaging Science Experiment (HiRISE) images and Digital Terrain Models (DTM). Based on the scenario of ground ice melting in a periglacial environment, we propose to test the hypothesis that Martian gullies on dunes are debris flows. This implies a flow with a significant proportion of liquid water (>10% in volume). We used an original method to study Martian gullies based on empirical equations from terrestrial debris flows in order to calculate the physical properties of Martians flows. We observe a decrease in viscosity induced by the relative increase of fluid concentration (from 28% to 39%) during the flow advance. The total estimated volume of eroded and deposited material range from ∼14850 m 3 to ∼18890 m 3. The volume of liquid water required to generate one gully ranges from 4450 m 3 to 6900 m 3. The calculated results for Martian gullies are consistent with terrestrial studies on debris flows. Based on a morphological description and on the estimated physical parameters, we propose a model for gully formation on Martian dunes. The melt water from near-surface ground ice is incorporated in the debris flow and water concentration increases during its propagation. The increase of water concentration in the debris flow can be explained by a progressive increase of water/ice content in the permafrost downstream. Consequently, the lack of a final deposit at the front of the gullies tends to demonstrate that the flow became relatively highly concentrated in liquid downstream and all the water could have been lost in the final stage of the flow. This process could explain the lack of terminal lobes at the front of the gullies. We conclude that a process of formation similar to terrestrial debris flows is plausible. The large amount of liquid water involved requires formation of Martian gullies on dunes during a warmer climatic episode. © 2012 Elsevier Ltd. All rights reserved.
Authors & Co-Authors
Jouannic, Gwenaël
France, Gif-sur-yvette
Université Paris-saclay
Italy, Chieti
University of G. D'annunzio Chieti and Pescara
Gargani, Julien
France, Gif-sur-yvette
Université Paris-saclay
Costard, F.
France, Gif-sur-yvette
Université Paris-saclay
Ori, Gian Gabriele
Italy, Chieti
University of G. D'annunzio Chieti and Pescara
Morocco, Marakech
Université Cadi Ayyad
Marmo, Chiara
France, Gif-sur-yvette
Université Paris-saclay
Schmidt, Frédéric
France, Gif-sur-yvette
Université Paris-saclay
Lucas, Antoine S.
United States, Pasadena
Division of Geological and Planetary Sciences
Statistics
Citations: 78
Authors: 7
Affiliations: 4
Identifiers
Doi:
10.1016/j.pss.2012.07.005
ISSN:
00320633
Research Areas
Environmental
Study Approach
Quantitative