Tables of Stark broadening profiles for the N V 6f, g, h-7f, g, h, i line complex at 4945A have been generated. Modern close-coupling techniques are used for the electron broadening while the important influence of perturbing ions is included within the framework of the model microfield method. Comparison has been made with the results of line formation calculations using approximate formulae for the Stark profiles.
The tables contain the area normalized Stark broadened spectral profiles of the HeI 492.2nm line. Doppler effect has not been included in the profiles. The first column of each table is the wavelength detuning, measured in nanometers, from the unperturbed wavelength. The other columns give the spectral profiles for different cases of perturber mass and electron temperature. Each table contains the data for a fixed electron density, ranging from 10^20^m^-3^ to 10^24^m^-3^ in different tables. Data corresponding to four different reduced masses of the emitter perturber pair, {mu}, are given in each table. The values of {mu} given in the tables are {mu}=0.8, 2.0, 4.0 and 10.0, in units of the proton mass. For each case of {mu} the profiles for different electron temperatures are given in different columns. Each table has a head giving the electron density value, and the values of {mu} and temperature corresponding to each column.
Using a semiclassical perturbation method, we have calculated electron-, proton-, and ionized helium-impact line widths and shifts for 52 Be III multiplets as a function of temperature and perturber density. Electron temperatures are 10000K; 20000K; 50000K; 100000K; 200000K and 300000K and perturber densities are from 10^11^cm^-3^ up to 10^21^cm^-3^. The obtained results have been used for discussion of regularities and systematic trends along spectral series.
Using the semiclassical perturbation approach, we have calculated electron-, proton-, He II-, Mg II-, Si II- and Fe II-impact line widths and shifts for 189 Ca I multiplets as a function of temperature and perturber density. Perturbers selected here are the main perturbers in solar atmospheres. Obtained results have been compared with the existing theoretical and experimental data.
We have determined matrix elements for all experimental configurations of CaIII, including the 3s^3^p^6^3d configuration. These values have been obtained using intermediate coupling (IC). For these IC calculations, we have used the standard method of least-squares fitting from the experimental energy levels, using the computer code developed by Robert Cowan. In this paper, using these matrix elements, we report the calculated values of the CaIII Stark widths and shifts for 148 spectral lines, of 56 CaIII spectral line transition probabilities and of eight radiative lifetimes of CaIII levels. The Stark widths and shifts, calculated using the Griem semi-empirical approach, correspond to the spectral lines of CaIII and are presented for an electron density of 10^17^cm^-3^ and temperatures T=1.0-10.0(x10^4^K). The theoretical trends of the Stark broadening parameter versus the temperature are presented for transitions that are of astrophysical interest. There is good agreement between our calculations, for transition probabilities and radiative lifetimes, and the experimental values presented in the literature. We have not been able to find any values for the Stark parameters in the references.
Using a semiclassical approach, we have calculated electron-, proton-, and He III-impact line widths and shifts for 4 Ca IX multiplets for perturber densities 10^18^-10^22^cm^-3^ and 48 Ca X multiplets for perturber densities 10^17^-10^22^cm^-3^. In both cases the temperature range is T=200000-5000000K. For lower perturber densities, obtained results are linear with perturber density.
Stark broadening parameters, widths, and shifts for 33 CdI singlets and 37 triplets were calculated using the semiclassical perturbation method. The results were compared with available experimental and theoretical data. Also, regularity in the spectral series 5s^2^ ^1^S-np ^1^P^o^ was investigated. The influence of Stark broadening was analyzed in A-type stellar atmospheres.
Stark broadening of the 18 Ga I transitions has been analyzed within the framework of the semiclassical perturbation method. Results obtained have been compared with available experimental and theoretical data and used for the consideration of the influence of the Stark broadening effect in stellar atmospheres