Abstract
Recent observations of the Hα contrast profiles of identifiable chromospheric fine structures are interpreted in terms of an empirical model. It is shown that the parameters inferred from an application of Beckers' ‘cloud’ model are unreliable, and the problem of line asymmetries is re-examined. Quantitative models for the Hα chromosphere near the limb suggest that the ‘dark band’ phenomenon is due to low opacity in the neighbourhood of the temperature minimum, while the peculiar appearance of mottle contrast profiles near the limb is explained in terms of foreground absorption.
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