Stark widths of Ar III spectral lines in the atmospheres of subdwarf B stars |
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| Authors: | Rafik Hamdi Nabil Ben Nessib Sylvie Sahal-Bréchot Milan S Dimitrijevi? |
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| Institution: | 1. Groupe de Recherche en Physique Atomique et Astrophysique, Faculté des Sciences de Bizerte, Université de Carthage, Tunisia;2. Deanship of the Foundation Year, Department of Physics, Umm Al-Qura University, PO Box 715, Makkah, Saudi Arabia;3. Department of Physics and Astronomy, College of Science, King Saud University, PO Box 2455, Riyadh 11451, Saudi Arabia;4. Laboratoire d’Étude du Rayonnement et de la Matière en Astrophysique, Observatoire de Paris, UMR CNRS 8112, UPMC, 5 Place Jules Janssen, 92195 Meudon Cedex, France;5. Astronomical Observatory, Volgina 7, 11060 Belgrade, Serbia |
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| Abstract: | Using semiclassical perturbation approach in impact approximation, we have calculated Stark widths for 32 spectral lines of doubly charged argon (Ar III). Oscillator strengths are calculated using Hartree–Fock method with relativistic correction (HFR) and an atomic model including 17 configurations. Energy levels are taken from NIST database. For perturbing levels for which the corresponding energy does not exist in NIST database, the calculated energies are used. Our widths are compared with the experimental results. The results presented here are of interest for modelling and investigation of stellar atmospheres since argon in different ionization stages is observed in many astrophysical objects. Finally, the importance of Stark broadening mechanism is studied in the atmospheric conditions of sdB stars. Electron impact Stark widths are compared to thermal Doppler widths as a function of temperature and optical depth of atmospheric layers. |
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| Keywords: | Atomic data Atomic processes Line: profiles Stars: atmospheres |
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