We consider the problem of influencing the motion of an electrically conducting fluid with an applied steady magnetic field. Since the flow is originating from buoyancy, heat transfer has to be included in the model. The stationary system of magnetohydrodynamics is considered, and an approximation of Boussinesq type is used to describe the buoyancy. The heat sources given by the dissipation of current and the viscous friction are not neglected in the fluid. The vessel containing the fluid is embedded in a larger domain, relevant for the global temperature- and magnetic field- distributions. Material inhomogeneities in this larger region lead to transmission relations for the electromagnetic fields and the heat flux on inner boundaries. In the presence of transparent materials, the radiative heat transfer is important and leads to a nonlocal and nonlinear jump relation for the heat flux. We prove the existence of weak solutions, under the assumption that the imposed velocity at the boundary of the fluid remains sufficiently small.
Different modes of magnetic field - chromospheric plasma interaction are possible under the assumption that the energy is released impulsively. One of them leads to the creation of
small-scale impulsive structures such as forced plume and dynamical stable current filaments. These structures we consider as basic MHD elements of the plasma of the solar active phenomena. We show that such a structuralization plays an important role in the process of solar surge formation and dynamics.