Stark Broadening of Several Ar I Spectral Lines in the Visible Spectrum

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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Stark Widths of Yb III and Lu IV Spectral Lines

Atoms ◽

10.3390/atoms7010010 ◽

2019 ◽

Vol 7 (1) ◽

pp. 10

Author(s):

Milan Dimitrijević

Keyword(s):

Experimental Data ◽

Rare Earth ◽

Rare Earth Elements ◽

Data Center ◽

Semiempirical Method ◽

Molecular Data ◽

Stellar Atmosphere ◽

Spectral Lines ◽

Stark Broadening ◽

Isoelectronic Sequence

Rare Earth Elements are important for stellar atmosphere analysis but the corresponding Stark broadening data are scarce. For Yb III and Lu IV theoretical as well as experimental data on Stark broadening parameters of spectral lines are absent in the literature. Using the modified semiempirical method of Dimitrijević and Konjević, we determined Stark widths for four Yb III and four Lu IV transitions, belonging to the erbium isoelectronic sequence. The obtained results are also used to discuss similarities between homologous transitions in the erbium isoelectronic sequence. We note as well that calculated widths will be implemented in the STARK-B database which is also a part of the Virtual Atomic and Molecular Data Center.

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Stark Broadening of In III Lines in Astrophysical and Laboratory Plasma

Open Astronomy ◽

10.1515/astro-2017-0347 ◽

2011 ◽

Vol 20 (4) ◽

Cited By ~ 1

Author(s):

Z. Simić ◽

M. S. Dimitrijević ◽

A. Kovačević ◽

S. Sahal-Bréchot

Keyword(s):

Experimental Data ◽

Perturbation Method ◽

Data Center ◽

White Dwarfs ◽

Charged Particles ◽

Molecular Data ◽

Spectral Lines ◽

Virtual Observatory ◽

Stark Broadening ◽

Laboratory Plasma

AbstractIn the deeper layers of hot stellar photospheres the Stark widths of spectral lines can be comparable and even larger than the thermal Doppler widths. Using the semiclassical perturbation method, we investigate the influence of the collisions with charged particles for the In III lines. We determine a number of Stark broadening parameters important in the atmospheres of A-type stars and white dwarfs. Also, the obtained results are compared with the available experimental data. The results will be included in the STARK-B database, the Virtual Atomic and Molecular Data Center and the Serbian Virtual Observatory.

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Stark Broadening of Several Ne II, Ne III and O III Spectral Lines for the Stark-B Database

Open Astronomy ◽

10.1515/astro-2017-0340 ◽

2011 ◽

Vol 20 (4) ◽

Cited By ~ 1

Author(s):

Milan S. Dimitrijević ◽

Andjelka Kovačević ◽

Zoran Simić ◽

Sylvie Sahal-Bréchot

Keyword(s):

Data Center ◽

Molecular Data ◽

Stellar Atmospheres ◽

Spectral Lines ◽

Stark Broadening ◽

Visible Part

AbstractIn order to complete Stark broadening data for Ne II and O III lines, needed for analysis of stellar atmospheres, we determined the missing parameters for the broadening by collisions with protons and ionized helium for 15 Ne II and 5 O III multiplets. Also, electron, proton and ionized helium impact broadening parameters for an important Ne II multiplet in the visible part of the spectrum and for three Ne III multiplets were calculated. The obtained data will be included in the STARK-B database, which is a part of the Virtual Atomic and Molecular Data Center.

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

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/stz1874 ◽

2019 ◽

Vol 488 (4) ◽

pp. 5594-5603 ◽

Cited By ~ 2

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.

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On the stark broadening of Os II spectral lines

Bulletin of Natural Sciences Research ◽

10.5937/bnsr10-27823 ◽

2020 ◽

Vol 10 (2) ◽

pp. 65-70

Author(s):

Milan Dimitrijević

Keyword(s):

Electron Density ◽

Spectral Lines ◽

Half Maximum ◽

Stark Broadening ◽

Plasma Parameters ◽

And Shifts

Stark broadening parameters, full widths at half maximum (FWHM) and shifts for 13 Os II lines have been calculated. The plasma parameters are: electron density of 1017 cm-3 and temperatures from 5 000 K to 80 000 K. Calculations have been performed with the simplified modified semiempirical (SMSE) approach. The results are also used for the consideration of Strak width and shift regularities within the Os II 6s6D-6p6Do multiplet.

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Measurement of Laser-Induced Plasma: Stark Broadening Parameters of Pb(II) 2203.5 and 4386.5 Å Spectral Lines

Applied Spectroscopy ◽

10.1177/0003702818816305 ◽

2019 ◽

Vol 73 (2) ◽

pp. 133-151 ◽

Cited By ~ 5

Author(s):

Aurelia Alonso-Medina

Keyword(s):

Yttrium Aluminum Garnet ◽

Electron Number Density ◽

Graphical Representation ◽

Spectral Lines ◽

Stark Broadening ◽

Number Density ◽

Electron Number ◽

Breakdown Spectroscopy ◽

Fundamental Wavelength ◽

And Shifts

In this work, the Stark broadening parameters (widths and shifts) of the 2203.5 Å and 4386.5 Å Pb(II) spectral lines have been investigated and measured in laser-induced breakdown spectroscopy (LIBS), using a lead sample (99.999% purity). A Q-switched neodymium-doped yttrium aluminum garnet (Nd:YAG) laser operating at its fundamental wavelength (10 640 Å), generating pulses of 290 mJ, 7 ns of duration, and a repeat frequency of 20 Hz, has been used for the ablation of said lead sample in vacuum and in a controlled argon atmosphere. A study to understand the expansion dynamics of the lead produced plasma was performed. The spectra have been obtained and measured at different time delays of the plasma evolution in the range of 0.15–9 μs, at which the temperature and electron number density are in the ranges of 28 200–8000 K and 1.3 × 1017 to 3 × 1015 cm−3, respectively. A graphical representation of the evolution of temperature and electron number density versus 0.3 to 6.5 μs delay from the laser pulse is presented. The important effect of the different environment where the plasma expands has been pointed out. Local thermodynamic equilibrium conditions have been checked. The obtained results of the Stark widths and shifts at the different temperatures and densities of electrons have been compared with the limited data available in the literature. This study aims to obtain more accurate values for these parameters and also to establish regularities and similarities for said parameters.

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Quantum Stark broadening of 3s–3p spectral lines in Li-like ions; Z-scaling and comparison with semi-classical perturbation theory

The European Physical Journal D ◽

10.1140/epjd/e2009-00167-8 ◽

2009 ◽

Vol 54 (1) ◽

pp. 51-64 ◽

Cited By ~ 20

Author(s):

H. Elabidi ◽

S. Sahal-Bréchot ◽

N. Ben Nessib

Keyword(s):

Perturbation Theory ◽

Spectral Lines ◽

Stark Broadening ◽

Classical Perturbation Theory

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ON THE STARK BROADENING OF Os II SPECTRAL LINES

University thought - Publication in Natural Sciences ◽

10.5937/univtho10-27823 ◽

2020 ◽

Vol 10 (2) ◽

Author(s):

Milan S. Dimitrijević

Keyword(s):

Electron Density ◽

Spectral Lines ◽

Half Maximum ◽

Stark Broadening ◽

Plasma Parameters ◽

And Shifts

Stark broadening parameters, full widths at half maximum (FWHM) and shifts for 13 Os II lines have been calculated. The plasma parameters are: electron density of 1017 cm-3 and temperatures from 5 000 K to 80 000 K. Calculations have been performed with the simplified modified semiempirical (SMSE) approach. The results are also used for the consideration of Strak width and shift regularities within the Os II 6s6D-6p6Do multiplet.

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On the Stark Broadening of Be II Spectral Lines

Data ◽

10.3390/data5040106 ◽

2020 ◽

Vol 5 (4) ◽

pp. 106

Author(s):

Milan S. Dimitrijević ◽

Magdalena Christova ◽

Sylvie Sahal-Bréchot

Keyword(s):

Perturbation Theory ◽

Plasma Diagnostics ◽

Spectral Lines ◽

Spectral Series ◽

Stark Broadening ◽

Stark Width

Calculated Stark broadening parameters of singly ionized beryllium spectral lines have been reported. Three spectral series have been studied within semiclassical perturbation theory. The plasma conditions cover temperatures from 2500 to 50,000 K and perturber densities 1011 cm−3 and 1013 cm−3. The influence of the temperature and the role of the perturbers (electrons, protons and He+ ions) on the Stark width and shift have been discussed. Results could be useful for plasma diagnostics in astrophysics, laboratory, and industrial plasmas.

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