scholarly journals Stark broadening parameter tables for Ne II and Ne III spectral lines

2001 ◽  
pp. 57-70 ◽  
Author(s):  
M.S. Dimitrijevic
Keyword(s):  
Stellar Atmospheres ◽  
Spectral Lines ◽  
Stark Broadening ◽  
Semiclassical Approach ◽  
Line Widths ◽  
And Shifts

Using a semiclassical approach, we have calculated electron-, proton-, He II-, Mg II-, Si II- and Fe II-impact line widths and shifts for 10 Ne II and 6 Ne III multiplets as a function of temperature and perturber density. For Ne II temperatures are: 5,000 K; 10,000 K; 20,000 K; 30,000 K; 50,000 K and 100,000 K and perturber densities from 1015 cm-3 up to 1020 cm-3. For Ne III temperatures are: 20,000 K; 50,000 K; 100,000 K; 200,000 K; 300,000 K and 500,000 K and perturber densities from 1017 cm-3 up to 1021 cm-3. Perturbers selected here, are the main perturbers in solar and stellar atmospheres.

scholarly journals Stark broadening parameter tables for neutral calcium spectral lines. I

1999 ◽  
pp. 35-74 ◽  
Author(s):  
M.S. Dimitrijevic ◽  
S. Sahal−Bréchot
Keyword(s):  
Stellar Atmospheres ◽  
Spectral Lines ◽  
Stark Broadening ◽  
Semiclassical Approach ◽  
Line Widths ◽  
And Shifts

Using a semiclassical approach, we have calculated electron?, proton?, He II?, Mg II-, Si II- and Fe II-impact line widths and shifts for 189 Ca I multiplets as a function of temperature. Perturbers selected here, are the main perturbers in solar and stellar atmospheres.

scholarly journals Stark broadening parameter tables for neutral zinc spectral lines

1999 ◽  
pp. 21-33 ◽  
Author(s):  
M.S. Dimitrijevic ◽  
S. Sahal−Bréchot
Keyword(s):  
Spectral Lines ◽  
Stark Broadening ◽  
Semiclassical Approach ◽  
Line Widths ◽  
And Shifts

Using a semiclassical approach, we have calculated electron?, proton? and He II?impact line widths and shifts for 32 Zn I multiplets as a function of temperature and perturber density.

scholarly journals The effect of hyperfine splitting on Stark broadening for three blue-green Cu i lines in laser-induced plasma

2019 ◽  
Vol 488 (4) ◽  
pp. 5594-5603 ◽  
Author(s):  
A M Popov ◽  
N I Sushkov ◽  
S M Zaytsev ◽  
T A Labutin
Keyword(s):  
Hyperfine Splitting ◽  
Stark Effect ◽  
Stellar Atmospheres ◽  
Spectral Lines ◽  
Stark Broadening ◽  
Laser Induced Plasma ◽  
Radiation Sources ◽  
And Shifts ◽  
First Time ◽  
Existing Data

ABSTRACT Stark effect is observed in many natural and artificial plasmas and is of great importance for diagnostic purposes. Since this effect alters profiles of spectral lines, it should be taken into account when assessing chemical composition of radiation sources, including stars. Copper is one of the elements which studies of stellar atmospheres deal with. To this end, UV and visible Cu lines are used. However, there is a lack of agreement between existing data on their Stark parameters. It is therefore of interest to obtain new experimental data on these lines and to compare them to previous results. In this work, we have estimated Stark widths and shifts for three blue-green lines at 5105.54, 5153.24, and 5218.20 Å (corresponding transitions are [3d104p] 2P° → [3d94s2] 2D and [3d104d] 2D → [3d104p] 2P°) observed in a ‘long-spark’ laser-induced plasma. For the first time, we have accurately estimated an impact of hyperfine splitting on the profile shapes of the studied lines taking also into account the isotope shifts. We have shown that both effects considerably influence shift and width of Cu i line at 5105.54 Å, and shifts of Cu i lines at 5153.24 and 5218.20 Å.

scholarly journals Stark broadening parameter tables for Kr VIII

1999 ◽  
pp. 73-77 ◽  
Author(s):  
M.S. Dimitrijevic ◽  
S. Sahal−Bréchot
Keyword(s):  
Stark Broadening ◽  
Semiclassical Approach ◽  
Line Widths ◽  
And Shifts

Using a semiclassical approach, we have calculated electron?, proton?, and He III?impact line widths and shifts for 6 Kr VIII multiplets as a function of temperature and perturber density.

scholarly journals Stark broadening parameter tables for Na X

1998 ◽  
pp. 65-91
Author(s):  
M.S. Dimitrijevic ◽  
S. Sahal−Bréchot
Keyword(s):  
Stark Broadening ◽  
Semiclassical Approach ◽  
Line Widths ◽  
And Shifts

Using a semiclassical approach, we have calculated electron?, proton?, and He III?impact line widths and shifts for 57 Na X multiplets as a function of temperature (200 000 K - 5 000 000 K) and perturber density (1017cm?3 - 1024cm?3.

scholarly journals Stark broadening parameter tables for Be III

2002 ◽  
pp. 67-88
Author(s):  
Milan Dimitrijevic ◽  
Miodrag Dacic ◽  
Zorica Cvetkovic ◽  
S. Sahal-Brechot
Keyword(s):  
Stark Broadening ◽  
Semiclassical Approach ◽  
Line Widths ◽  
And Shifts

Using a semiclassical approach, we have calculated electron-, proton-, and He II-impact line widths and shifts for 52 Be III multiplets as a function of temperature and perturber density. The electron temperatures are 10,000 K 20,000 K; 50,000 K; 100,000 K 200,000K and 300,000 K and perturber densities are from 10(exp)11 cm(exp)-3 up to 10(exp)21 cm(exp)-3.

scholarly journals Stark broadening parameter tables for Ar VIII

1999 ◽  
pp. 15-20 ◽  
Author(s):  
M.S. Dimitrijevic ◽  
S. Sahal−Bréchot
Keyword(s):  
Stark Broadening ◽  
Semiclassical Approach ◽  
Line Widths ◽  
And Shifts

Using a semiclassical approach, we have calculated electron?, proton?, and He III?impact line widths and shifts for 9 Ar VIII transitions as a function of temperature and perturber density.

scholarly journals Theoretical Stark Broadening Parameters for UV–Blue Spectral Lines of Neutral Vanadium in the Solar and Metal-Poor Star HD 84937 Spectra

Atoms ◽  
2020 ◽  
Vol 8 (4) ◽  
pp. 64
Author(s):  
Cristóbal Colón ◽  
María Isabel de Andrés-García ◽  
Lucía Isidoro-García ◽  
Andrés Moya
Keyword(s):  
Spectral Lines ◽  
Matrix Elements ◽  
Stark Broadening ◽  
Laboratory Plasma ◽  
Hartree Fock ◽  
The Matrix ◽  
Line Widths ◽  
And Shifts ◽  
Semi Empirical ◽  
Metal Poor Star

Using Griem’s semi-empirical approach, we have calculated the Stark broadening parameters (line widths and shifts) of 35 UV–Blue spectral lines of neutral vanadium (V I). These lines have been detected in the Sun, the metal-poor star HD 84937, and Arcturus, among others. In addition, these parameters are also relevant in industrial and laboratory plasma. The matrix elements required were obtained using the relativistic Hartree–Fock (HFR) method implemented in Cowan’s code.

scholarly journals Stark broadening parameter tables for F VI and Cl VII

1998 ◽  
pp. 93-101
Author(s):  
M.S. Dimitrijevic ◽  
S. Sahal−Bréchot
Keyword(s):  
Stark Broadening ◽  
Semiclassical Approach ◽  
Line Widths ◽  
And Shifts

Using a semiclassical approach, we have calculated electron?, proton?, and He III?impact line widths and shifts for 2 F VI and 10 Cl VII multiplets as a function of temperature and perturber density.

scholarly journals Comparisons and Comments on Electron and Ion Impact Profiles of Spectral Lines

2011 ◽  
Vol 20 (4) ◽  
Author(s):  
Sylvie Sahal-Bréchot ◽  
Milan S. Dimitrijević ◽  
Nebil Ben Nessib
Keyword(s):  
Neutral Atom ◽  
Molecular Data ◽  
Stellar Atmospheres ◽  
Spectral Lines ◽  
Stark Broadening ◽  
Spectroscopic Diagnostics ◽  
Data Centre ◽  
Ion Impact ◽  
And Shifts ◽  
The Impact

AbstractStark broadening theory is currently operated for calculating widths and shifts of spectral lines that are needed for spectroscopic diagnostics and modeling in astrophysics, laboratory and technological plasmas. We have calculated a great number of data, obtained through the impact semiclassical perturbation theory: tables have been published for neutral atom and ion emitters, and typical temperatures, electron and ion densities. They are currently implemented in the STARK-B database which participates in the European effort within the Virtual Atomic and Molecular Data Centre. Despite of that, a great number of data are still missing. In the present paper, we revisit and compare a great number of the impact Stark widths and shifts by considering their semiclassical perturbation expressions. We also provide fitting formulae which are essential for the modeling codes of stellar atmospheres and envelopes.

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