Abstract
The significance of Stark broadening for Solar and stellar plasma research is discussed. Since the influence of Stark broadening within a spectral series increases with the increase of the principal quantum number of the upper level, the Stark broadening contribution may become significant for Rydberg atoms and ions where the optical electron is weakly bound to the core. Consequently, e.g. high member Balmer series lines may be used for Solar plasma diagnostic. The importance of Stark broadening for sub photospheric layers modelling is discussed also. The methods and results developed and obtained on Belgrade Astronomical Observatory and in Serbia are principally discussed .
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