Mechanisms for MHD Poynting flux generation in simulations of solar photospheric magneto-convection
arXiv:1206.0030 · doi:10.1088/2041-8205/753/1/L22
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.
5 pages, 5 figures, accepted for ApJL
References in corpus (7)
- A solar surface dynamo
- Magneto-convection in a sunspot umbra
- Convectively driven vortex flows in the Sun
- The horizontal internetwork magnetic field: numerical simulations in comparison to observations with Hinode
- Vortices, shocks, and heating in the solar photosphere: effect of a magnetic field
- Stokes diagnostics of simulated solar magneto-convection
- Decay of a simulated mixed-polarity magnetic field in the solar surface layers
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