Stark Widths of Ar II Spectral Lines in the Atmospheres of Subdwarf B Stars

Hamdi, Rafik; Nessib, N. Ben; Dimitrijević, M. S.

doi:10.3390/atoms5030026

Cited by 19 publications

(13 citation statements)

References 25 publications

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“…For example, the agreement with Djurović et al (2013) was 27% for 4p-4d transitions except for four transitions. Concerning Stark widths, the comparison with experiments is made in Hamdi et al (2017Hamdi et al ( , 2018 for 212 spectral lines and we found an agreement generally good. For example, the average agreement for 4p-4d transitions was 10% comparing with Djurović et al (2013) and 20% comparing with Pellerin et al (1997).…”

Section: Resultssupporting

confidence: 68%

On the semiclassical perturbation Stark shifts of Ar II spectral lines

Hamdi¹,

Nessib²,

Sahal‐Bréchot³

et al. 2020

caosp

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We present in this paper Stark shifts as a function of temperature for 20 spectral lines of Ar II belonging to 4p -4d transition array. Calculations are made using semiclassical perturbation approach in impact approximation. Atomic data used in this calculation are carried out using Hartree-Fock method with relativistic corrections. Singly charged argon (Ar II) spectral lines are observed in many astrophysical plasmas. Ar II spectral lines are also important for laboratory plasmas and laser physics and technology.

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Section: Resultssupporting

confidence: 68%

On the semiclassical perturbation Stark shifts of Ar II spectral lines

Hamdi¹,

Nessib²,

Sahal‐Bréchot³

et al. 2020

caosp

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“…We compare our results (Q and SCP SST ) to the SCP calculations (SCP BD ) performed in [12], where atomic data have been taken from the method of Bates and Damgaard [13]. This method has been used many times with different ions, and it has been shown that the corresponding results (using the Bates and Damgaard or the SST data) are in good agreement with experimental and other theoretical results [31][32][33]. Many of these SCP results have been stored in the database STARK-B [34].…”

Section: Line Broadening Resultsmentioning

confidence: 60%

Quantum and Semiclassical Stark Widths for Ar VII Spectral Lines

Aloui

Elabidi

Dimitrijević

2018

Atoms

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We present in this paper the results of a theoretical study of electron impact broadening for several lines of the Ar VII ion. The results have been obtained using our quantum mechanical method and the semiclassical perturbation one. Results are presented for electron density 10 18 cm −3 and for electron temperatures ranging from 2 × 10 4 to 5 × 10 5 K required for plasma modeling. Our results have been compared to other semiclassical ones obtained using different sources of atomic data. A study of the strong collisions contributions to line broadening has been performed. The atomic structure and collision data used for the calculations of line broadening are also calculated by our codes and compared to available theoretical results. The agreement found between the two calculations ensures that our line broadening procedure uses adequate structure and collision data.

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“…In order to introduce corrections to the widths and shifts due to the difference between calculated and experimental wavelengths, equation ( 8) of Hamdi et al (2013) has been used. Previously, we have checked the accuracy of our method by comparing our results with experimental data (Hamdi et al 2017(Hamdi et al , 2018(Hamdi et al , 2019.…”

Section: The Methodsmentioning

confidence: 99%

Stark broadening effect in hot DA white dwarfs: Ultraviolet lines of Fe V

et al. 2021

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Stark widths and shifts have been calculated for 17 ultraviolet lines of Fe V of astrophysical interest. The calculations have been made using semiclassical perturbation approach. The work is motivated by the importance of ultraviolet lines for the study of hot white dwarf atmospheres specially for investigations of the variation of fine structure constant in strong gravitational field. Our Stark broadening parameters are presented for a range of temperature from 50,000 to 600,000 K. Our results are used to investigate the importance of electron impact broadening in plasma conditions of hot DA white dwarfs. Electron impact Stark width is compared to Doppler width as a function of atmospheric layer temperature and as a function of logarithm of Rosseland optical depth.

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Stark Widths of Ar II Spectral Lines in the Atmospheres of Subdwarf B Stars

Cited by 19 publications

References 25 publications

On the semiclassical perturbation Stark shifts of Ar II spectral lines

On the semiclassical perturbation Stark shifts of Ar II spectral lines

Quantum and Semiclassical Stark Widths for Ar VII Spectral Lines

Stark broadening effect in hot DA white dwarfs: Ultraviolet lines of Fe V

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