Abstract
Data for Stark full widths at half maximum for 46 Co II multiplets were calculated using a modified semiempirical method. In order to show the applicability and usefulness of this set of data for research into white dwarf and A type star atmospheres, the obtained results were used to investigate the significance of the Stark broadening mechanism for Co II lines in the atmospheres of these objects. We examined the influence of surface gravity (log g), effective temperature and the wavelength of the spectral line on the importance of the inclusion of Stark broadening contribution in the profiles of the considered Co II spectral lines, for plasma conditions in atmospheric layers corresponding to different optical depths.
Highlights
The importance of Co II spectral lines, weak or strong, for the cobalt abundance determination in the spectra of A to F type stars, has been discussed elsewhere [1]
We examined the influence of surface gravity, effective temperature and the wavelength of the spectral line on the importance of the inclusion of Stark broadening contribution in the profiles of the considered Co II spectral lines, for plasma conditions in atmospheric layers corresponding to different optical depths
It is noticed that disregarding the Stark broadening effect in the process of spectral line synthesis can produce a worse fit of synthetic with observed spectral lines, or can cause errors in abundance determination, especially for A-type stars ([6], for example)
Summary
The importance of Co II spectral lines, weak or strong (weak lines of Co II could help in the better adjustment of cobalt abundance measured on the basis of existing strong Co I lines), for the cobalt abundance determination in the spectra of A to F type stars, has been discussed elsewhere [1] For this reason, Stark full widths at half maximum for 46 Co II multiplets have been calculated [2,3] to be helpful for astrophysical purposes. Stark broadening of the lines in the spectra of hot and dense celestial objects such as white dwarfs (WD), because of specific conditions of high electron density and high temperature in their atmospheres, usually dominates on Doppler broadening.
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