On the Nature of the Chromosphere-Corona Transition Region of the Solar Atmosphere

TL;DR

This paper investigates the temperature distribution in the solar atmosphere's transition region, showing that classical heat conduction applies under both slow and impulsive heating conditions, with implications for understanding solar atmospheric structure.

Contribution

It provides a theoretical analysis of temperature and emission measure distributions in the solar transition region under different heating scenarios, confirming the applicability of classical heat conduction.

Findings

Classical collisional heat conduction is valid in the transition region.

Temperature distribution depends on radiation loss and thermal conductivity.

Results apply to both slow and impulsive heating cases.

Abstract

The distribution of temperature and emission measure in the stationary heated solar atmosphere was obtained for the limiting cases of slow and fast heating, when either the gas pressure or the concentration are constant throughout the layer depth. Under these conditions the temperature distribution with depth is determined by radiation loss and thermal conductivity. It is shown that both in the case of slow heating and of impulsive heating, temperatures are distributed in such a way that classical collisional heat conduction is valid in the chromosphere-corona transition region of the solar atmosphere.