The H Emission of Prominences

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Abstract
It is shown that Hα radiation from the solar disk is strongly reflected by prominences and is an important component of their radiation. An analysis of their observed Hα emission at the limb indicates a range of kinetic temperatures of about |${10}^{4}\,\text{to}\,2\times{10}^{4}$| deg. K and electron concentrations of about |${10}^{10}\,\text{to}\,5\times{10}^{10}\,\text{cm}^{-3}$| for stable prominences. Two alternative explanations are given for the double peaked profiles of Hα sometimes observed in solar prominences, depending on whether scattering is coherent or incoherent.

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