Simulation of Amazonis Planitia Summer Convection

Details Simulation of Amazonis Planitia Summer Convection Simulation of Amazonis Planitia Summer Convection

Dec 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agufm.p51a0337m&link_type=abstract

American Geophysical Union, Fall Meeting 2002, abstract #P51A-0337

Physics

5409 Atmospheres: Structure And Dynamics, 5445 Meteorology (3346), 6225 Mars

Scientific paper

Numerous large dust devils have been repeatedly observed by Viking and MGS MOC during the summer season in northern Amazonis Planitia. The presence and size of these vortices strongly suggests that the daytime atmosphere over the region vigorously convects at this season. Of course, the convection itself is intangible to spacecraft. The Mars Regional Atmospheric Modeling System (MRAMS), a mesoscale numerical model, can provide the linkage between such observed phenomena and those that are invisible. The MRAMS simulation presented here provides a three-dimensional view of how the atmosphere over Amazonis Planitia evolves with time (about 0.5 sol) and interacts with mesoscale surface features (e.g., ridges, craters) and atmospheric phenomena (e.g., katabatic flows from Olympus Mons, topography-induced gravity waves). These results are also compared to information derived from the MOC dust devil images.

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