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Geology; March 2008; v. 36; no. 3; p. 211-214; DOI: 10.1130/G24346A.1
© 2008 Geological Society of America
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Recent bright gully deposits on Mars: Wet or dry flow?

Jon D. Pelletier*,1, Kelly J. Kolb2, Alfred S. McEwen2 and Randy L. Kirk3

1 Department of Geosciences, University of Arizona, Tucson, Arizona 85721, USA
2 Department of Planetary Sciences, University of Arizona, Tucson, Arizona 85721, USA
3 United States Geological Survey, Astrogeology Program, 2255 N Gemini Drive, Flagstaff, Arizona 86001, USA


Figure 01
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  		Figure 1. Two-dimensional model results and input data sets. A: Slope contour map, slope color map, shaded relief map, and portion of High Resolution Imaging Science Experiment (HiRISE) image (PSP_001714_1415) of initiation and runout zone of bright gully deposit in Centauri Montes region discovered by Malin et al. (2006) (see footnote 1). The slope map was spatially averaged before contouring to minimize microtopographic variability. B: Color maps of peak depth and velocity for the best-fit liquid water case with fluid-loss rate of 0.77 mm/s. C: Color maps of peak depth and velocity for dry granular case.

 

Figure 02
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  		Figure 2. One-dimensional kinematic model results for dry granular flow. A: Along-channel elevation and slope angle of bright gully deposit (data extracted from photogrammetric digital elevation model), as function of distance from initiation point, with deposit margin indicated. B: Model predictions for velocity of the granular flow as function of distance for three different combinations of flow thickness and median grain size. Thicker and finer-grained flows have longer runout distances. C: Yield stress {tau}y and dynamic viscosity {eta} corresponding to the model examples in B, according to equation 2.

 




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