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We investigate the generation mechanisms of MHD Poynting flux in themagnetised solar photosphere. Using radiative MHD modelling of the solarphotosphere with initial magnetic configurations that differ in their fieldstrength and geometry, we show the presence of two different mechanisms for MHDPoynting flux generation in simulations of solar photosphericmagneto-convection. The weaker mechanism is connected to vertical transport ofweak horizontal magnetic fields in the convectively stable layers of the upperphotosphere, while the stronger is the production of Poynting flux in stronglymagnetised intergranular lanes experiencing horizontal vortex motions. Thesemechanisms may be responsible for the energy transport from the solarconvection zone to the higher layers of the solar atmosphere.

Mechanisms for MHD Poynting flux generation in simulations of solar photospheric magneto-convection