Stark broadening of the 447.1nm line of neutral helium in a weakly coupled plasma has been studied. This spectral line has a very close forbidden component. This means it is very sensitive to the plasma electron density, which is similar to hydrogen lines, for which the Stark effect is linear. The aim of this work is to supply information to be used in the spectroscopic diagnostics of plasmas.
New tables of Stark broadened hydrogen Lyman, Balmer and Paschen lines are presented for a wide range of plasma conditions, allowing the complete spectrum of these series to be modelled up to the Inglis Teller limit. The formalism, based on the Model Microfield Method (MMM) for both the electronic and ionic broadenings , gives an accurate description of the line profile from the centre to the wings. The profiles are calculated for a pure hydrogen plasma. All the transitions from n_lower = 1 (Lyman), 2(Balmer), 3(Paschen) to n_upper= (2 to 30) Lyman, (3 to 30) Balmer, (4 to 30) Paschen are reported. The temperature range is 2500 to 1.259E+06 K (10 temperatures) The electronic density range is 10e10 to 3.162E+19 (20 densities) A summary of the parameter values is reported in file "params.dat". The line profiles are tabulated in directories: ly/lyNN for Lyman lines, with NN = 02 .. 30 ba/baNN for Balmer lines, with NN = 03 .. 30 pa/paNN for Paschen lines, with NN = 04 .. 30 Each TRANSITION directory (for example ly/ly02, for Lyman{alpha}) contains at maximum 20 files, denoted by profilX.dat, ie, profil1.dat, ..., profil20.dat, which correspond to different increasing densities. Due to the plasma lowering of the ionization limit (Inglis Teller limit), the number of reported density calculations decreases when NN increases. The number of density files profilX.dat is reported for each transition directory in the file nraie.dat.
With the development of space-borne spectroscopy, spectral line parameters for a large number of lines become of increasing interest for astrophysics. To provide Stark broadening data for ion lines from complex spectra, we present here calculated Stark widths for 37 Kr II lines from the 5s-5p transition. The calculations were performed by using a modified semiempirical approach. The obtained Stark widths are on average in satisfactory agreement with available experimental data.
By using the semiclassical-perturbation formalism, we have calculated electron-, proton-, and He III-impact line widths and shifts for 4 K VIII and 30 K IX multiplets, of interest for analysis, investigation and modeling of different plasmas in solar and stellar subphotospheric layers research and plasma physics. The obtained results are presented as a function of temperature and perturber density. Results are compared with other theoretical estimates, based on regularities and systematic trends.
The electron - impact line widths and shifts for 16 Mn II, 3 Mn III, 10 Ga III, 8 Ge III and 14 Ge IV multiplets, have been considered within a modified semiempirical approach. Moreover, using a semiclassical approach, we have considered electron-, proton-, and He III-impact line widths and shifts for 3 Ge IV multiplets. The obtained results have been compared with other theoretical results.
Using a semiclassical perturbation approach, we have calculated electron-, proton-, and He III-impact line widths and shifts for 57 Na X multiplets for perturber densities 10^17^-10^24^cm^-3^ and temperatures T=200000-5000000K. For lower perturber densities, the Stark broadening parameters are proportional to the perturber density.
Using a semiclassical perturbation approach, we have calculated electron-, proton-, and He III-impact line widths and shifts for 14 O VII and 18 Mg XI multiplets. For O VII, perturber densities are 10^17^-10^23^cm^-3^ and temperatures T=100000-2000000K. For Mg XI, perturber densities are 10^18^-10^24^cm^-3^ and temperatures T=500000-5000000K. For lower perturber densities, the Stark broadening parameters are proportional to the perturber density.
Using a semi-empirical approach, we report in this paper calculated values of the Stark broadening parameters for 58 lines of PbIV. They were calculated using a set of wavefunctions obtained from Hartree-Fock relativistic calculations including core polarization effects. Stark widths for 58 lines of PbIV arising from 5d^10^ns (n=7,8), 5d^10^6p, 5d^9^6s6p, 5d^10^nd (n=6,7), 5d^10^5g and 5d^10^nh (n=6,7) configurations have been calculated in this way. Stark widths and shifts are presented for an electron density of 10^17^cm^-3^ and temperatures T=11000-200000K. These atomic data are relevant to the analysis of PbIV detected in Far Ultraviolet Spectroscopic Explorer spectra of hot subdwarf B stars and are used to determine the lead abundance of the early B main-sequence star AV 304 in the Small Magallanic Cloud by measuring the 1313.1{AA} resonance line. Common trends for the Stark width of the resonance lines have been found and are discussed.
Using a semiclassical approach, we have calculated electron-, proton-, and He III-impact line widths and shifts for 114 P IV multiplets for perturber densities 10^15^-10^20^cm^-3^ and temperatures T=5000-1000000K. The obtained results have been compared with results obtained by using various simpler approaches.
By using the semiclassical-perturbation formalism, we have calculated electron-, proton-, and He III-impact line widths and shifts for 4 Sc X, 10 Sc XI, 4 Ti XI and 27 Ti XII multiplets, significant for analysis, investigation and modeling of different plasmas in solar and stellar physics, physics and technology. The results are presented as a function of temperature and perturber density.