摘要：Thermal convection of the Martian lower atmosphere is examined by the use of a two-dimensional anelastic model with a resolution fine enough to describe convection eddies. For a homogeneous radiative cooling of 50 K/day given in the layer below 5 km, a layer of time-dependent convection develops up to about 6 km in height. The intensity of realized vertical winds ranges up to 20 m/s. The dust, which is injected into the lowest layer and treated as a passive tracer, is transported immediately in the convection layer and mixed uniformly. The intensity of the horizontal winds near the surface reaches about 10 m/s, which, combined with large-scale motions, is expected to contribute to the dust injection into the atmosphere.
