Temperature structure of the chromosphere-corona transition region

Abstract

Starting from the formula for line intensities E for a spherically symmetric atmosphere, considering the pressure parameter P 0 = N e T e to be constant the inverse temperature gradient can be determined by taking it out from the integral for E . In this way Dupree and Goldberg (1967) found that the temperature gradient varies considerably whereas the conductive flux factor F =T e 5/2 (dT e /d h ) is nearly constant for T e above 10 5 K. The best fit was obtained by using photospheric abundances. As the inverse temperature gradient varies considerably in the line forming region, it is, however, not satisfactory to take it out from the integral.