Stark Widths of Ar II Spectral Lines in the Atmospheres of Subdwarf B Stars
Rafik Hamdi,
Nabil Ben Nessib,
Sylvie Sahal Bréchot,
Milan S. Dimitrijević
Affiliations
Rafik Hamdi
Deanship of the Foundation Year, Department of Physics, Umm Al-Qura University, Makkah 24382, Saudi Arabia
Nabil Ben Nessib
Department of Physics and Astronomy, College of Science, King Saud University, PO Box 2455, Riyadh 11451, Saudi Arabia
Sylvie Sahal Bréchot
LERMA, Observatoire de Paris, PSL Research University, CNRS, Sorbonne Universités, UPMC (Univ. Pierre & Marie Curie), Paris 06, 5 Place Jules Janssen, 92190 Meudon, France
Milan S. Dimitrijević
LERMA, Observatoire de Paris, PSL Research University, CNRS, Sorbonne Universités, UPMC (Univ. Pierre & Marie Curie), Paris 06, 5 Place Jules Janssen, 92190 Meudon, France
Stark broadening parameters are of interest for many problems in astrophysics and laboratory plasmas investigation. Ar II spectral lines are observed in many kinds of stellar atmospheres such as the atmospheres of B-Type stars and subdwarf B stars. In this work, we present theoretical Stark widths for Ar II spectral lines. We use the impact semiclassical perturbation approach. Our results are compared with the available experimental values. Finally, the importance of the Stark broadening mechanism is studied in atmospheric conditions of subdwarf B stars.
