  We investigate the generation mechanisms of MHD Poynting flux in the
magnetised solar photosphere. Using radiative MHD modelling of the solar
photosphere with initial magnetic configurations that differ in their field
strength and geometry, we show the presence of two different mechanisms for MHD
Poynting flux generation in simulations of solar photospheric
magneto-convection. The weaker mechanism is connected to vertical transport of
weak horizontal magnetic fields in the convectively stable layers of the upper
photosphere, while the stronger is the production of Poynting flux in strongly
magnetised intergranular lanes experiencing horizontal vortex motions. These
mechanisms may be responsible for the energy transport from the solar
convection zone to the higher layers of the solar atmosphere.
