A model for the penumbral fine structure and the Evershed flow

Assuming that the interchange convection of mag- netic flux elements is the physical cause for the existence of filamentary penumbrae in sunspots, we investigate the behavior of an individual fibril embedded in the deep penumbra. The fibril is approximated by a thin magnetic flux tube which evolves dy- namically in the environment given by the global magnetostatic model of a sunspot. Our simulation shows that the flux tube, initially positioned at the penumbra-quiet Sun boundary in the model, will rise through its deep penumbra developing a flow along the tube that points upward beneath the photosphere, and radially out- ward above the photosphere. Our results suggest that a bright filament may be formed by an extended tail of a penumbral grain. Such filaments are optically thick, hotter than the surroundings, and elevated above a darker background. An upflow in penum- bral grains bends horizontally outwards above the photosphere and gradually cools down due to radiative losses leading to a tail that gradually darkens. The plasma flow inside the flux tube then becomes transparent and the tube constitutes a thin elevated flow channel, that can reproduce the observed features of the Ever- shed effect. We present also a new acceleration mechanism for the Evershed flow. It is demonstrated that a local surplus of gas pressure develops inside the tube as it rises through the specific (superadiabatic and magnetized) penumbral background. The resulting gradient of the gas pressure can drive the flow along the tube.