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

TL;DR

This study identifies two distinct mechanisms for MHD Poynting flux generation in the solar photosphere, involving magnetic field transport and vortex motions, which could explain energy transfer to higher solar atmospheric layers.

Contribution

The paper reveals two different mechanisms for MHD Poynting flux generation in solar photospheric magneto-convection simulations, highlighting their roles in energy transport.

Findings

Vertical transport of horizontal magnetic fields in upper photosphere.

Poynting flux production in magnetised intergranular lanes.

Mechanisms may explain energy transfer to the solar atmosphere.

Abstract

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.