Results 21 to 30 of about 597,270 (283)
Stark broadening for Br VI and Kr V-VII lines in hot star atmospheres
Astronomy & Astrophysics, 2021 Context. This paper provides missing Stark broadening of the Br VI and Kr V-VII lines recently discovered in the ultraviolet spectrum of the hot white dwarf RE 0503–289 and investigates the importance of the Stark broadening mechanism versus the Doppler ...
S. Sahal-Bréchot, H. Elabidi
semanticscholar +1 more source
Stark broadening of Be II spectral lines [PDF]
Journal of Quantitative Spectroscopy and Radiative Transfer, 1992 Using a semiclassical approach, we have calculated electron-, proton-, and ionized helium-impact line widths and shifts for 101 In II multiplets. The resulting data have been compared with existing experimental and theoretical values.
Milan S Dimitrijević +1 more
openaire +1 more source
Stark Broadening of Zn III Spectral Lines
Universe, 2022 Stark widths for spectral lines within 24 multiplets of Zn III singlets and triplets have been calculated using modified semiempirical method for an electron density of 1017 cm−3 and temperatures from 5000 K up to 100,000 K.
Milan S. Dimitrijević +1 more
doaj +1 more source
Stark broadening of UV nickel lines [PDF]
Space Science Reviews, 1972 Widths of Stark broadened Ni I Lines in the spectral range of 3000 Å–4000 Å have been measured using a gas driven shock tube as a spectroscopic source. Electron densities were determined using measured pressure and temperature data. Within the density range 6 × 1016 cm-3 to 12 × 1016 cm-3 the observed widths were linear functions of the electron ...
Roger D. Bengtson +2 more
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Hβ Stark broadening in cold plasmas with low electron densities calibrated with Thomson scattering
Spectrochimica Acta, Part B: Atomic Spectroscopy, 2012 Antonio Sola +2 more
exaly +2 more sources
Hydrogen Stark Broadened Brackett lines [PDF]
International Journal of Spectroscopy, 2010 Stark-broadened lines of the hydrogen Brackett series are computed for the conditions of stellar atmospheres and circumstellar envelopes. The computation is performed within the Model Microfield Method, which includes the ion dynamic effects and makes the bridge between the impact limit at low density and the static limit at high density and in the ...
Stehlé, C., Fouquet, S.
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Stark broadening parameter tables for Kr VIII [PDF]
Serbian Astronomical Journal, 1999 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.
Dimitrijević M.S., Sahal−Bréchot S.
doaj +1 more source
Quantifying the statistical noise in computer simulations of Stark broadening
, 2020 Computer simulations employed in Stark broadening calculations are reexamined within the perspective of giving error bars to results. As a rule, the calculated spectra exhibit a noisy structure, which is inherent to the random number generators involved ...
J. Rosato, Y. Marandet, R. Stamm
semanticscholar +1 more source
Stark broadening parameter tables for Be III [PDF]
Serbian Astronomical Journal, 2002 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
Dimitrijević Milan S. +3 more
doaj +1 more source
Stark broadening parameter tables for Na X [PDF]
Serbian Astronomical Journal, 1998 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.
Dimitrijević M.S., Sahal−Bréchot S.
doaj +1 more source