  With the adaptation of the FLASH code we simulate magnetohydrodynamic-gravity
waves and vortices as well as their response in the magnetized
three-dimensional (3D) solar atmosphere at different heights to understand the
localized energy transport processes. In the solar atmosphere strongly
structured by gravitational and magnetic forces, we launch a localized velocity
pulse (in horizontal and vertical components) within a bottom layer of 3D solar
atmosphere modelled by initial VAL-IIIC conditions, which triggers waves and
vortices. The rotation direction of vortices depends on the orientation of an
initial perturbation. The vertical driver generates magnetoacoustic-gravity
waves which result in oscillations of the transition region, and it leads to
the eddies with their symmetry axis oriented vertically. The horizontal pulse
excites all magnetohydrodynamic-gravity waves and horizontally oriented eddies.
These waves propagate upwards, penetrate the transition region, and enter the
solar corona. In the high-beta plasma regions the magnetic field lines move
with the plasma and the temporal evolution show that they swirl with eddies. We
estimate the energy fluxes carried out by the waves in the magnetized solar
atmosphere and conclude that such wave dynamics and vortices may be significant
in transporting the energy to sufficiently balance the energy losses in the
localized corona. Moreover, the structure of the transition region highly
affects such energy transports, and causes the channelling of the propagating
waves into the inner corona.
