A Discussion on the physics of the solar atmosphere - A magnetic model of the solar transition region

Abstract

A two-dimensional model of the chromosphere and corona has been constructed. This is based upon the magnetic flux concentrations which occur at the boundaries of the supergranule convection cells. The expansion of the magnetic flux is determined by the vertical extent of the convecting plasma. The distribution of atmospheric material is consistent both with observed spectral intensities and with energy balance requirements. The model predicts a primary transition region which is confined to an area about 10" wide overlying the supergranule boundaries. A secondary transition region which is much thinner covers the cell centres. The predictions are fully consistent with recent ultraviolet observations.