Laboratory Simulations of Martian and Venusian Aeolian Processes

Details Laboratory Simulations of Martian and Venusian Aeolian Processes Laboratory Simulations of Martian and Venusian Aeolian Processes

May 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999stin...9961887g&link_type=abstract

Technical Report, Arizona State Univ. Tempe, AZ United States Dept. of Geology

Mathematics

Logic

Mars Atmosphere, Mars Surface, Venus (Planet), Venus Atmosphere, Venus Surface, Wind (Meteorology), Wind Effects, Wind Erosion, Simulation, Mariner 9 Space Probe, Pioneer Venus Spacecraft, Radar Imagery, Soviet Spacecraft, Venera Satellites, Viking Mars Program, Titan, Triton

Scientific paper

With the flyby of the Neptune system by Voyager, the preliminary exploration of the Solar System was accomplished. Data have been returned for all major planets and satellites except the Pluto system. Results show that the surfaces of terrestrial planets and satellites have been subjected to a wide variety of geological processes. On solid- surface planetary objects having an atmosphere, aeolian processes are important in modifying their surfaces through the redistribution of fine-grained material by the wind. Bedrock may be eroded to produce particles and the particles transported by wind for deposition in other areas. This process operates on Earth today and is evident throughout the geological record. Aeolian processes also occur on Mars, Venus, and possibly Titan and Triton, both of which are outer planet satellites that have atmospheres. Mariner 9 and Viking results show abundant wind-related landforms on Mars, including dune fields and yardangs (wind-eroded hills). On Venus, measurements made by the Soviet Venera and Vega spacecraft and extrapolations from the Pioneer Venus atmospheric probes show that surface winds are capable of transporting particulate materials and suggest that aeolian processes may operate on that planet as well. Magellan radar images of Venus show abundant wind streaks in some areas, as well as dune fields and a zone of possible yardangs. The study of planetary aeolian processes must take into account diverse environments, from the cold, low-density atmosphere of Mars to the extremely hot, high- density Venusian atmosphere. Factors such as threshold wind speeds (minimum wind velocity needed to move particles), rates of erosion and deposition, trajectories of windblown particles, and aeolian flow fields over various landforms are all important aspects of the problem. In addition, study of aeolian terrains on Earth using data analogous to planetary data-collection systems is critical to the interpretation of spacecraft information and places constraints on results from numerical models and laboratory simulations.

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