Laboratory simulations of Martian gullies on sand dunes
Article first published online: 4 NOV 2008
Copyright 2008 by the American Geophysical Union.
Geophysical Research Letters
Volume 35, Issue 21, November 2008
How to Cite
2008), Laboratory simulations of Martian gullies on sand dunes, Geophys. Res. Lett., 35, L21501, doi:10.1029/2008GL035638., , , and (
- Issue published online: 4 NOV 2008
- Article first published online: 4 NOV 2008
- Manuscript Accepted: 24 SEP 2008
- Manuscript Revised: 18 SEP 2008
- Manuscript Received: 20 AUG 2008
 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.