PROMINENCE MODEL BASED ON SPECTRAL OBSERVATIONS

Intensities and profiles of the H α, H β, H γ, K, and D3 lines are measured in a solar prominence. From the profiles of these lines we estimate T = 6400 K and υt = 5.7 km s-1. We construct a simple isothermal model which explains the H α intensity and profile for an assumed total particle density nT = 3 × 1011 cm-3, and a filling factor, α = 1/6. From this model we find that the source function in the H α line is nearly constant through the prominence. We estimate from the model that the radiative energy loss at the center of the prominence is of the order of 107 erg s-1 g-1. © 1979 D. Reidel Publishing Co.