On the Problem of Heat Transport in the Solar Atmosphere

Abstract

AbstractIn the context of the problem of energy transport in the solar atmosphere, we present new results on physical properties of a transition region between the hot and cold plasma in quiet regions and in flares. In quiet regions, the transition region between the corona and chromosphere is shown to be a very thin layer, in which however the classical collisional approach is valid very well. A stability of the transition region is investigated. It is shown to be stable, moreover it is a stable consequence of the thermal instability in the condensation mode regime. We have developed also mathematical models for describing plasma heating in the corona and chromosphere by heat fluxes from a super-hot reconnecting current layer. It is shown that applicability conditions of classical heat conduction are not valid in the flare transition region and at the higher temperatures. Models, that account the effect of collisional relaxation, describe heat transport in flares better than Fourier’s law. A possibility of comparing theoretical and observational data is discussed.KeywordsSolar FlareThermal WaveCurrent LayerMagnetic TubeQuiet RegionThese keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.