Stark Broadening of N VI Spectral Lines

Stark broadening parameters, line widths and shifts, for 15 N VI multiplets are calculated using semiclassical perturbation theory for temperatures from 50,000 K to 2,000,000 K, and perturber density of 1016 cm−3. As perturbers have been taken electrons, protons and He III ions (alpha particles), wh...

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Bibliographic Details
Published in:Universe (Basel) 2023-12, Vol.9 (12), p.511
Main Authors: Dimitrijević, Milan S., Christova, Magdalena D., Sahal-Bréchot, Sylvie
Format: Article
Language:English
Subjects:
Accretion disks
Astronomical research
Astrophysics
Atmosphere
atomic data
atomic processes
Boron
Charged particles
Ions
Lasers
line profiles
N VI
Neutron stars
Neutrons
Nitrogen
Perturbation (Mathematics)
Physics
Plasma
proton-boron fusion
Satellites
Space telescopes
Spectrum analysis
Stark broadening
Temperature
White dwarfs
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Summary:Stark broadening parameters, line widths and shifts, for 15 N VI multiplets are calculated using semiclassical perturbation theory for temperatures from 50,000 K to 2,000,000 K, and perturber density of 1016 cm−3. As perturbers have been taken electrons, protons and He III ions (alpha particles), which are of interest particularly for white dwarfs. Moreover, B III, B IV, B V and B VI ions have been taken as well, due to their significance for proton-boron fusion investigations. An example of the importance of Stark broadening in comparison with thermal Doppler broadening in atmospheres of spectral class DO white dwarfs is also presented. The obtained results are of interest particularly for white dwarf atmospheres modelling and analysis and synthesis of their spectra as well as for laser driven plasma in proton-boron fusion investigations.
ISSN:2218-1997
2218-1997
DOI:10.3390/universe9120511