Abstract
A summary of spectroscopic and atomic physics results that were obtained in the last 30 years and are closely related to diagnostics of solar plasmas will be presented. The article will not review the very extensive work that was done on the theoretical determinations of energy levels, transition probabilities, or calculations of excitation ionization and recombination cross sections, but with the end results of these calculations. In other words it deals with line intensities, line shapes and their changes as a result of the properties of the plasma from which they are emitted.
The emission lines under discussion are optically thin and the spectral range covered is primarily from 2000 Å down to 1.8 Å. The review is divided into several sections according to the typical wavelength ranges covered by the different spectrometers.
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