Systematic trends of Stark broadening parameters with spectroscopic charge <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" altimg="si31.svg"><mml:mi>Z</mml:mi></mml:math> within the neon isoelectronic sequence from Mg III to Br XXVI

Elabidi, Haykel

doi:10.1016/j.jqsrt.2020.107407

Cited by 6 publications

(5 citation statements)

References 24 publications

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“…This method has been applied many times Aloui et al 2018;Elabidi & Sahal-Bréchot 2019;Aloui et al 2019b,a) and has given good results compared to other approaches. It has been used also to study several physics problems like fine structure effects (Elabidi et al 2009), strong collisions and quadrupolar potential contributions to Stark broadening (Elabidi et al 2014), scaling of line widths with temperature and ionic charge Elabidi & Sahal-Bréchot 2019;Elabidi 2021a). In Elabidi (Elabidi 2021a), the calculation of new Stark broadening of about 160 lines for eight neon-like ions, and the investigation of the systematic trend of Stark broadening 𝑤 with the spectroscopic charge 𝑍, allowed us to establish a linear relation between log(𝑤) and log(𝑍).…”

Section: III Si Ii Iii and Al Iii Line Widthsmentioning

confidence: 99%

Quantum mechanical line widths of ionized oxygen, silicon, and aluminium; comparisons with recent experimental results

Elabidi

Sahal‐Bréchot

Dimitrijević

et al. 2023

Monthly Notices of the Royal Astronomical Society

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We present in this paper new quantum Half Widths at Half intensity Maximum (HWHM) for 101 spectral lines of the following ions: O II (35 lines), O III (20 lines), Si II (9 lines), Si III (12 lines) and Al III (25 lines). The present quantum results are compared to new experimental ones. No previous quantum calculations have been performed for these ions. The relatively high differences found between the new and previous measurements and the available theoretical calculations encourage us to conduct these quantum calculations. Our quantum method has been used many years ago and has given good results compared to other approaches, so it can be a useful tool to check the new experimental results, or to understand the disagreement found for some lines. Furthermore, the obtained results can be used for the abundance determination of elements, the calculation of stellar opacity, the interpretation and modelling of stellar spectra, and the estimation of the relative transfer through stellar plasmas, etc. Part of the present results will be also implemented to the database of Stark broadening parameters STARK-B.

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Section: III Si Ii Iii and Al Iii Line Widthsmentioning

confidence: 99%

Quantum mechanical line widths of ionized oxygen, silicon, and aluminium; comparisons with recent experimental results

Elabidi

Sahal‐Bréchot

Dimitrijević

et al. 2023

Monthly Notices of the Royal Astronomical Society

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“…For example, Smiljanic et al [17] investigated aluminium abundances in giants and dwarfs and their implications on stellar and galactic chemical evolution using two samples: i) more than 600 dwarfs of the solar neighborhood and of open clusters and ii) low-and intermediate-mass clump giants in six open clusters. Carretta et al [18] determined aluminium abundances for 90 red giant branch (RGB) stars in NGC 2808, and Smith [19] derrived atmospheric abundance of aluminium for a sample of forty normal, superficially normal, and HgMn type main-sequence late-B stars Recently, Elabidi [21] used quantum mechanical theory [22,23] to calculate 20 Al IV lines belonging to 2p 6 -3s, 3s-3p and 3p-3d transitions. All these lines are in UV but in astronomy are particularly convenient spectral lines in the visible.…”

Section: Introductionmentioning

confidence: 99%

Stark Broadening of Al IV Spectral Lines

Dimitrijević¹,

Christova²

2023

Preprint

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Stark widths for 23 transitions in Al IV have been calculated employing modified semiempirical method. The results are obtained for an electron density of 10^17 cm−3 and temperatures from 10,000 K up to 160,000 K. The results obtained in this investigation are used for the examination of the influence of Stark broadening in Al IV stellar spectra, as well as to check Stark width regular behavior and similarites within Al IV spectrum.

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“…One of the first studies dealing with Stark broadening of aluminum spectral lines is presented in Mazing et al (1964) and since than a great number of studies of Stark broadening of spectral lines of aluminum in different ionization degrees, witnessing on its importance, have been published. The needs for Stark broadening data for spectral lines of aluminum ions in astrophysics stimulated particularly the efforts on that subject (Dimitrijević;Sahal-Bréchot, 1994;Elabidi, 2021). For example results for 7 Al XI spectral lines for perturber densities 10 18 cm −3 -10 23 cm −3 and temperatures: 500 000 K -4 000 000 K are provided in Dimitrijević and Sahal-Bréchot (1994).…”

Section: Introductionmentioning

confidence: 99%

“…For example results for 7 Al XI spectral lines for perturber densities 10 18 cm −3 -10 23 cm −3 and temperatures: 500 000 K -4 000 000 K are provided in Dimitrijević and Sahal-Bréchot (1994). Elabidi (2021) calculated Stark broadening parameters for 20 Al IV lines in UV, belonging to 2p 6 -3s, 3s-3p and 3p-3d transitions. For calculations he used quantum mechanical theory (Elabidi, 2004;Elabidi et al, 2008), while in Dimitrijević and Sahal-Bréchot (1994), the semiclassical perturbation formalism (Sahal-Bréchot, 1969 a b) is applied.…”

Section: Introductionmentioning

confidence: 99%