Abstract
For the purpose of investigating fundamental features of thermal convection in the Martian atmosphere, a three-dimensional non-hydrostatic model for the Martian atmosphere is developed and a numerical simulation is performed. The governing equations of the model are based on the quasi-compressible system. The turbulent mixing coefficient is calculated by using a prognostic equation ofsubgrid scale turbulent energy and the surface flux is estimated by using bulk method. As a preliminary experiment, convection is generated by horizontally uniform heating whose profile is given from a result of a one-dimensional radiative convective equilibrium model. The convective field which can be regarded to be in a statically equilibrium state is examined.