Abstract
Using the semi-classical perturbation approach in the impact approximation, full width at half maximum and shift have been determined for eight spectral lines of Ar VII, for broadening by electron-, proton-, and He III-impacts. The results are provided for temperatures from 20,000 K to 500,000 K, and for an electron density of 10 18 cm − 3 . The obtained results will be included in the STARK-B database, which is also in the virtual atomic and molecular data center (VAMDC).
Highlights
With the development of space astronomy and satellite-born spectroscopy, trace elements—which have been without importance for astrophysics— become increasingly important, and the corresponding data of interest for the analysis of stellar spectra
Full widths at half intensity maximum (FWHM) W and shifts d for eight additional transitions have been calculated by using semiclassical perturbation method (SCP, [4,5]) for collisions of Ar VII ions with electrons, protons, and He III ions, since hydrogen and helium are the main constituents of stellar atmospheres
The semiclassical perturbation formalism (SCP) applied here for the calculations of Stark broadening parameters, full width at half intensity maximum (FWHM-W), and shift of spectral line (d) has been formulated in [4,5], and later updates, optimisations, and innovations are presented in Sahal-Bréchot [6], Sahal-Bréchot [7], Dimitrijević et al [8], Dimitrijević and Sahal-Bréchot [9], and Sahal-Bréchot et al [10]
Summary
With the development of space astronomy and satellite-born spectroscopy, trace elements—which have been without importance for astrophysics— become increasingly important, and the corresponding data of interest for the analysis of stellar spectra. Werner et al [2] have found Ar VII lines in some of the hottest known central stars of planetary nebulae, with the effective temperatures of 95,000–110,000 K, and in (pre-). White dwarfs by analyzing high-resolution spectra from the Far Ultraviolet Spectroscopic Explorer (FUSE). We note that Stark broadening is the principal pressure broadening mechanism in such hot stars, and without the corresponding Stark broadening data, reliable analysis and modelling of high-resolution spectra are not possible. Concerning Stark broadening parameters for Ar VII spectral lines, there is only one article where. Stark broadening parameters are provided for three transitions [3]. Full widths at half intensity maximum (FWHM) W and shifts d for eight additional transitions have been calculated by using semiclassical perturbation method (SCP, [4,5]) for collisions of Ar VII ions with electrons, protons, and He III ions, since hydrogen and helium are the main constituents of stellar atmospheres
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