Trajectories and energy transfer of saltating particles onto rock surfaces: Application to abrasion and ventifact formation on Earth and Mars

• Published in: Journal of Geophysical Research - Planets Vol. 110; no. E12; pp. E12004 - n/a
• Main Authors: Bridges, Nathan T., Phoreman, James, White, Bruce R., Greeley, Ronald, Eddlemon, Eric E., Wilson, Gregory R., Meyer, Christine J.
• Format: Journal Article
• Language: English
• Published: American Geophysical Union 01-12-2005; Blackwell Publishing Ltd
• Subjects: aeolian processes; Atmospheric Processes; Boundary layer processes; Erosion and weathering; Mars; Planetary Sciences; Solar System Objects; Solid Surface Planets; Surface materials and properties; ventifacts; wind abrasion; wind abrasion; ventifacts; aeolian processes
• ISSN: 0148-0227; 2156-2202
• DOI: 10.1029/2004JE002388

The interaction between saltating sand grains and rock surfaces is assessed to gauge relative abrasion potential as a function of rock shape, wind speed, grain size, and planetary environment. Many kinetic energy height profiles for impacts exhibit a distinctive increase, or kink, a few centimeters above the surface, consistent with previous field, wind tunnel, and theoretical investigations. The height of the kink observed in natural and wind tunnel settings is greater than predictions by a factor of 2 or more, probably because of enhanced bouncing off hard ground surfaces. Rebounded grains increase the effective flux and relative kinetic energy for intermediate slope angles. Whether abrasion occurs, as opposed to simple grain impact with little or no mass lost from the rock, depends on whether the grain kinetic energy (EG) exceeds a critical value (EC), as well as the flux of grains with energies above EC. The magnitude of abrasion and the shape change of the rock over time depends on this flux and the value of EG > EC. Considering the potential range of particle sizes and wind speeds, the predicted kinetic energies of saltating sand hitting rocks overlap on Earth and Mars. However, when limited to the most likely grain sizes and threshold conditions, our results agree with previous work and show that kinetic energies are about an order of magnitude greater on Mars.