Electron impact broadening and atomic data for As IV-V, Mo V and In V spectral lines

• Published in: Journal of quantitative spectroscopy & radiative transfer 2024-08, Vol.322, p.109027, Article 109027
• Main Authors: Aloui, R., Elabidi, H., Dimitrijević, M.S., Sahal-Bréchot, S.
• Format: Article
• Language: English
• Subjects: Line profiles-atomic data-atomic processes-atmospheres-stars-white dwarfs; Sciences of the Universe
• ISSN: 0022-4073; 1879-1352
• DOI: 10.1016/j.jqsrt.2024.109027

Missing Stark broadening parameters for 33 spectral lines of several arsenic, molybdenum and indium ions (7 As IV, 4 As V, 12 Mo V and 10 In V lines) have been calculated using a quantum-mechanical method. All the considered spectral lines for As IV and As V have been detected for the first time in the atmospheres of cool DO white dwarfs HD 149499 B and p=HZ 21, these four As V lines that have been discovered in HD 149499 B are also present in the UV spectrum of hot white dwarf (WD) RE 0503−289. All the considered spectral lines for Mo V have been recently discovered for the first time in the ultraviolet (UV) spectrum of the DO-type white dwarf (WD) RE 0503−289. Also, the ten considered lines for In V have been detected in the ultraviolet (UV) spectrum of the DO-type white dwarf (WD) RE 0503−289, that five among those discovered — recently — for the first time. This recent discovery encourages us to calculate their Stark widths to fill the lack of the data base STARK-B and for use in investigations of observed spectra in such stars. Before the Stark widths evaluation, two calculation steps have been carried out : in the first step, we calculate the atomic structure and then the electron-ion collision as a second step using the sequence of the codes (superstructure, distorted wave, and jajom) of University College London. We provide our results for these lines at different temperature values and at density Ne=1017 cm−3. •Stark broadening calculations for 7 As IV, 4 As V, 12 Mo V and 10 In V lines using a quantum mechanical method.•Evaluation the atomic radiative parameters (energy levels, transition probabilities, line strengths...) using the UCL codes, which are entered to the line broadening calculations.•The motivation of our work is the recent discovery of the new As IV, As V, Mo V and In V spectral lines in the atmospheres of cool DO white dwarfs HD 149499 B and HZ 21 and in the UV spectrum of hot white dwarf RE 0503-289.•Therefore, in the literature, no other results have been found for the Stark broadening to compare with them.•Our results can fill the lack in the STARK-B database, which is accessible for the astrophysicists.