Abstract
We use a system of univelocity equations for a multi-phase fluid as a description of the Mars atmosphere to achieve a better understanding of the dependence of the structure and governing mechanisms of the mesoscale processes on the thermal andorographic inhomogeneities and on dust transport. The major advantage of using this particular type of equations is that it allows us to describe uniformily the atmospheric flow over mountains, craters and sandy surfaces. This lets us to analyse the structure of wind flows over complex terrain in the important case of non-stationary conditions of dust lifting and dust deposition.
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