Abstract
The properties of closed coronal loops are reviewed. First we discuss the main features of the static, hot loop models. In these models thermal conduction plays the dominant role in determining the temperature and density structure. Next the cool loop models and their implications for solar observations are discussed. Finally, some new theoretical results on coronal abundances are presented. It is argued that chromospheric evaporation, which is a basic feature of the hot models, can account for the observed anomalies in the coronal element abundances.
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