Energy fluxes escaping the solar atmosphere are computed for the 2-1 and 3-I lines of H, He I, and He ii and for certain subordinate transitions for He I and He ii, using a new technique recently developed by Athay (1965a). Good agreement with observed fluxes is obtained with a relatively simple model chromosphere consistent with the fluxes observed in He I singlets and triplets observed at eclipse and with radio data. It is shown that local density increases in spicules and plages will produce increased brightness in the 2-1 lines and in the subordinate lines of He I and He ii. The 3-1 lines tend to be formed higher in the atmosphere than the 2-1 lines, particularly for He ii, and they show smaller increases in brightness associated with local increases in density than do the 2-1 lines. Local changes in temperature result in relatively weak change in the intensities of H and He I lines.
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R. G. Athay (1965) studied this question.