Abstract
A dynamical, homogeneous model of the chromosphere-corona transition region and of the lower corona is presented, based on the hydrodynamical equations and on a semi-empirical relation deduced from radio observations. The model is shown to be in agreement with radio and UV observations and with the particle flux given by solar wind measurements. A comparison with the analogous static model shows that dynamical effects are very small.
From the model it is possible to give an estimate of the energy dissipated at each level by the waves that propagate in the solar atmosphere. It is shown that this energy source cannot be neglected with comparison to the usual conductive, convective and radiative sources. The importance of the kinetic energy flux connected with the spicules is also discussed.
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Chiuderi, C., Riani, I. A dynamical model for the chromosphere-corona transition region. Sol Phys 34, 113–124 (1974). https://doi.org/10.1007/BF00149603
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DOI: https://doi.org/10.1007/BF00149603