Laboratory simulations of Martian gullies on sand dunes

Small gullies, observed on Mars, could be formed by groundwater seepage from an underground aquifer or may result from the melting of near‐surface ground ice at high obliquity. To test these different hypotheses, a cold room‐based laboratory simulation has been performed. The experimental slope was...

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Bibliographic Details
Published in:Geophysical research letters 2008-11, Vol.35 (21), p.L21501-n/a
Main Authors: Védie, E., Costard, F., Font, M., Lagarde, J. L.
Format: Article
Language:English
Subjects:
Debris flow and landslides
Earth Sciences
Earth, ocean, space
Exact sciences and technology
Geomorphology
Geophysics
gullies
hillslope
Hydrology
Instruments and techniques
Mars
modeling
Planetary Sciences
Sciences of the Universe
simulations
Solar System Objects
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Summary:Small gullies, observed on Mars, could be formed by groundwater seepage from an underground aquifer or may result from the melting of near‐surface ground ice at high obliquity. To test these different hypotheses, a cold room‐based laboratory simulation has been performed. The experimental slope was designed to simulate debris flows on sand dune slopes at a range of angles, different granulometry and permafrost characteristics. Preliminary results suggest that the typical morphology of gullies observed on Mars can best be reproduced by the formation of linear debris flows related to the melting of a near‐surface ground ice with silty materials. This physical modelling highlights the role of the periglacial conditions, especially the active‐layer thickness during debris‐flow formation.
ISSN:0094-8276
1944-8007
DOI:10.1029/2008GL035638