THE HYDROGEN SPECTRUM OF MODEL PROMINENCES

The emission of hydrogen lines and continua from solar prominences is investigated using a set of 140 simple models, covering the range of p hysical conditions usually assumed for these objects. These models are plane-parallel, isobaric and isothermal. The computations have been c arried out using a 20 level plus continuum hydrogen atom, and taking i nto account the effects of partial frequency redistribution in the Lym an-alpha and beta lines. The aim of these computations is twofold: Fir stly, to describe the variations of hydrogen lines and continua emitte d by prominences when physical conditions vary. Secondly, to provide o bservers with some diagnostic tool to interpret data such as intensity ratios, line widths, etc... The results of computations are given as mixed table-figure panels, each of them corresponding to a given model and summarizing the associated physical parameters and the principal features of the emitted hydrogen spectrum. Finally, for some specific parameters (or couple of parameters), we present figures illustrating the variations of these quantities across the whole set of models.