scholarly journals Stark broadening data tables for some analogous spectral lines along Li and Be isoelectronic sequences

1999 ◽  
pp. 65-72 ◽  
Author(s):  
M.S. Dimitrijevic
Keyword(s):  
Spectral Lines ◽  
Experimental Results ◽  
Oscillator Strengths ◽  
Perturbation Approach ◽  
Stark Broadening ◽  
Resonance Contribution ◽  
Data Tables ◽  
Coulomb Approximation ◽  
Selection Of

By using the semiclassical perturbation approach, Stark broadening parameters due to the interaction with a selection of perturbers of interest for recently published experimental results for Li - like B III, C IV, N V and O VI 3s2S-3p2Po, and for Be - like B II, C III, N IV and O V 3s3S-3p3Po multiplets, have been calculated. The results are presented as a function of temperature for a perturber density of 1017cm?3. The influence of resonance contribution for B II, differences in Stark broadening parameters if we take oscillator strengths calculated within the Coulomb approximation or taken from TOP Database, and the influence of transitions with different parent terms, have been discussed as well.

Ab Initio Determination of Atomic Structure and Stark Broadening Parameters: Pb IV and Recent Results

2011 ◽  
Vol 20 (4) ◽  
Author(s):  
R. Hamdi ◽  
N. Ben Nessib ◽  
M. S. Dimitrijević ◽  
S. Sahal-Bréchot
Keyword(s):  
Ab Initio ◽  
Atomic Structure ◽  
Energy Levels ◽  
Relativistic Effects ◽  
Spectral Lines ◽  
Oscillator Strengths ◽  
Perturbation Approach ◽  
Stark Broadening ◽  
Relativistic Approach

AbstractWe present a review of our previous ab initio calculations of Stark broadening parameters using semi-classical perturbation method for the calculation of Stark widths and shifts, and the SUPERSTRUCURE (SST) code for the determination of atomic structure. SST code takes into account the configuration interactions and relativistic effects. New results are also presented for some spectral lines of Pb IV. Energy levels and oscillator strengths are calculated using Hartree-Fock relativistic approach, and the Stark broadening parameters are determined using a semiclassical perturbation approach.

scholarly journals Stark broadening parameter tables for In II

2000 ◽  
pp. 57-90 ◽  
Author(s):  
M.S. Dimitrijevic ◽  
S. Sahal-Brechot
Keyword(s):  
Spectral Lines ◽  
Perturbation Approach ◽  
Stark Broadening

Electron-, proton-, and ionized helium-impact broadening parameter tables for In II spectral lines, are presented as a function of the temperature and the perturber density. Calculations have been performed within the semiclassical perturbation approach.

scholarly journals Stark broadening parameter tables for neutral calcium spectral lines, II

2000 ◽  
pp. 39-88 ◽  
Author(s):  
M.S. Dimitrijevic ◽  
S. Sahal-Brechot
Keyword(s):  
Spectral Lines ◽  
Perturbation Approach ◽  
Stark Broadening

Electron-, proton-, and ionized helium-impact broadening parameter tables for neutral calcium spectral lines, have been presented as a function of the temperature and the perturber density. Calculations have been performed within the semiclassical perturbation approach.

The chemical composition of the sun1This review is part of a Special Issue on the 10th International Colloquium on Atomic Spectra and Oscillator Strengths for Astrophysical and Laboratory Plasmas.

2011 ◽  
Vol 89 (4) ◽  
pp. 327-331 ◽  
Author(s):  
N. Grevesse ◽  
M. Asplund ◽  
A.J. Sauval ◽  
P. Scott
Keyword(s):  
Chemical Elements ◽  
Molecular Data ◽  
Solar Neighborhood ◽  
Spectral Lines ◽  
Oscillator Strengths ◽  
Atomic Data ◽  
Solar Photosphere ◽  
International Colloquium ◽  
Laboratory Plasmas ◽  
Selection Of

We have very recently re-determined the abundances of nearly all the available chemical elements in the solar photosphere, from lithium to thorium (Asplund et al. Annu. Rev. Astron. Astrophys. 47, 481 (2009)). This new complete and homogeneous analysis results from a very careful selection of spectral lines of all the indicators of the abundances present in the solar photospheric spectrum, from a discussion of the atomic and molecular data, and from an analysis of these lines based on a new 3D model of the solar outer layers, taking non-LTE effects into account when possible. We present these new results, compare them with other recent solar data as well as with recent results for the solar neighborhood, and discuss some of their most important implications as well as some of the atomic data we still urgently need.

scholarly journals Semiclassical perturbation Stark shifts of singly charged argon spectral lines

2019 ◽  
Vol 488 (2) ◽  
pp. 2473-2479
Author(s):  
Rafik Hamdi ◽  
Nabil Ben Nessib ◽  
Sylvie Sahal-Bréchot ◽  
Milan S Dimitrijević
Keyword(s):  
Energy Levels ◽  
Relativistic Correction ◽  
Spectral Lines ◽  
Oscillator Strengths ◽  
Perturbation Approach ◽  
Hartree Fock ◽  
Calculated Energy ◽  
Impact Approximation ◽  
Singly Charged ◽  
Experimental Values

AbstractUsing semiclassical perturbation approach in impact approximation, Stark shifts for singly charged argon (Ar ii) spectral lines have been calculated. Energy levels and oscillator strengths needed for this calculation were determined using Hartree–Fock method with relativistic correction (HFR). We compare our results with experimental values for 100 spectral lines. We also present results as a function of temperature for 161 spectral lines for collisions with electrons, protons, singly charged helium and singly charged argon. This work extends our previous one.

scholarly journals The Belgian repository of fundamental atomic data and stellar spectra (BRASS)

2019 ◽  
Vol 624 ◽  
pp. A60 ◽  
Author(s):  
M. Laverick ◽  
A. Lobel ◽  
P. Royer ◽  
T. Merle ◽  
C. Martayan ◽  
...  
Keyword(s):  
Quality Assessment ◽  
Large Scale ◽  
Spectral Lines ◽  
Oscillator Strengths ◽  
Atomic Data ◽  
Chemical Abundance ◽  
Stellar Spectra ◽  
Atomic Lines ◽  
The Universe ◽  
Selection Of

Context. Fundamental atomic transition parameters, such as oscillator strengths and rest wavelengths, play a key role in modelling and understanding the chemical composition of stars in the universe. Despite the significant work under way to produce these parameters for many astrophysically important ions, uncertainties in these parameters remain large and can limit the accuracy of chemical abundance determinations.Aims. The Belgian repository of fundamental atomic data and stellar spectra (BRASS) aims to provide a large systematic and homogeneous quality assessment of the atomic data available for quantitative spectroscopy. BRASS shall compare synthetic spectra against extremely high-quality observed spectra, at a resolution of ∼85 000 and signal-noise ratios of ∼1000, for approximately 20 bright BAFGK spectral-type stars, in order to critically evaluate the atomic data available for over a thousand potentially useful spectral lines.Methods. A large-scale homogeneous selection of atomic lines is performed by synthesising theoretical spectra of literature atomic lines for FGK-type stars including the Sun, resulting in a selection of 1091 theoretically deep and unblended lines in the wavelength range 4200–6800 Å, which may be suitable for quality assessment. Astrophysical log(g f) values are determined for the 1091 transitions using two commonly employed methods. The agreement of these log(g f) values are used to select well-behaved lines for quality assessment.Results. We found 845 atomic lines to be suitable for quality assessment, of which 408 were found to be robust against systematic differences between analysis methods. Around 53% of the quality-assessed lines were found to have at least one literature log(g f) value in agreement with our derived values, though the remaining values can disagree by as much as 0.5 dex. Only ∼38% of Fe Ilines were found to have sufficiently accurate log(g f) values, increasing to ∼70–75% for the remaining Fe-group lines.

scholarly journals On Stark Broadening of Heavy Element Lines in A-Type Star Spectra: Bi II Lines

1993 ◽  
Vol 138 ◽  
pp. 165-168
Author(s):  
M. S. Dimitrijević ◽  
L. Č. Popović
Keyword(s):  
Ionization Potential ◽  
Heavy Element ◽  
Spectral Lines ◽  
Experimental Results ◽  
Strong Absorption ◽  
Type Star ◽  
Stark Broadening ◽  
Correct Knowledge ◽  
Semiempirical Approach

AbstractWe report here results of Bi II spectral lines Stark broadening research within the modified semiempirical approach. The strong absorption Bi II lines observed in Hg – Mn star atmospheres have been investigated as well as the influence of the departure from LS – coupling and the correct knowledge of ionization potential. The obtained results have been compared with other estimations and with experimental results.

scholarly journals Stark Broadening of Isolated Lines from Multiply Charged Ions

1977 ◽  
Vol 43 ◽  
pp. 24-24
Author(s):  
J. D. Hey
Keyword(s):  
Spectral Lines ◽  
Oscillator Strengths ◽  
Stark Broadening ◽  
Multiply Charged Ions ◽  
Multiply Charged ◽  
Configuration Mixing ◽  
Lower Temperature ◽  
The Relationship ◽  
Bound Electrons ◽  
Charged Ions

When calculating the Stark widths of isolated lines of multiply charged ions with several bound electrons, radiated by dense, hot plasmas, the existing theories of Stark broadening which have been applied mainly to lower-temperature measurements on singly-ionized species, need to be modified in several respects. These modifications involve taking more careful account of the complexities of the particular atomic structure: e.g. deviations from LS coupling, configuration mixing, and optically forbidden transitons. Earlier work, showing explicitly the relationship between the Stark widths and the oscillator strengths for the collision-induced transitions Which contribute to the width, is extended. Some of the principles involved will be discussed and, if time permits, comparison will be made between calculations and the results of several critically selected experiments on spectral lines in the near UV (2000-3500 Å).

Recent progress in spectroscopy of tungsten1This review is part of a Special Issue on the 10th International Colloquium on Atomic Spectra and Oscillator Strengths for Astrophysical and Laboratory Plasmas.

2011 ◽  
Vol 89 (5) ◽  
pp. 551-570 ◽  
Author(s):  
A. Kramida
Keyword(s):  
Energy Levels ◽  
Experimental Studies ◽  
Theoretical Data ◽  
Theoretical Work ◽  
Spectral Lines ◽  
Oscillator Strengths ◽  
International Colloquium ◽  
10Th International Colloquium ◽  
Laboratory Plasmas ◽  
Data Tables

This contribution reviews experimental and theoretical work on spectroscopy of tungsten published since the last critical compilation of the energy levels and spectral lines of highly ionized tungsten (Kramida and Shirai. At. Data Nucl. Data Tables, 95, 305 (2009)). Since then, 18 new experimental studies were published, which resulted in new identifications and (or) significantly improved wavelengths of spectral lines and energy levels of Li-like through As-like and Pm-like tungsten. A few tens of theoretical studies of tungsten spectra were published since 2008. A number of them report on high-precision calculations of energy levels, transition wavelengths, and radiative rates for tungsten spectra, such as neutral tungsten, Yb-like, Rh-like through Rb-like, Ag-like, Ga-like, Zn-like, Ni-like, Ca-like, Al-like, Mg-like, Na-like, Ne-like, B-like, Be-like, and Li-like. These developments are reviewed. Based on new experimental data, systematic errors are removed from some of the earlier measurements. Some new data are obtained by analyzing publications of other authors. Based on new published theoretical data, some old experimental results were confirmed and assessed. Revised and extended tables of energy levels and spectral lines of highly ionized tungsten are presented.

Sign in / Sign up

Export Citation Format

Share Document