Stark widths and shifts for spectral lines of Sn iv

Stark Broadening of Se IV, Sn IV, Sb IV and Te IV Spectral Lines

“…There is no experimental or theoretical data for comparison for Se IV, Sb IV and Te IV. For Sn IV exist four transitions where the comparison with semiempirical data of de Andrés-García et al [21] is possible, while for other two there is no theoretical or experimental data in literature. There are two reasons to calculate Stark broadening for four tansitions already calculated by de Andrés-García et al [21].…”

“…For Sn IV exist four transitions where the comparison with semiempirical data of de Andrés-García et al [21] is possible, while for other two there is no theoretical or experimental data in literature. There are two reasons to calculate Stark broadening for four tansitions already calculated by de Andrés-García et al [21]. The first step is to compare with their results and to see if a systematic difference exist, so that user who needs also data for two transitions not calculated by [21], could eventualy perform the corresponding scaling or correction.…”

“…There are two reasons to calculate Stark broadening for four tansitions already calculated by de Andrés-García et al [21]. The first step is to compare with their results and to see if a systematic difference exist, so that user who needs also data for two transitions not calculated by [21], could eventualy perform the corresponding scaling or correction. The second reason is to check large difference between Stark widths within the multiplet 5p 2 P o -6s 2 S. For four transitions, existing in the paper of de Andrés-García et al [21] we performed calculations for temperatures given in this article and compared the corresponding FWHM in Table 2.…”

“…Results of theoretical calculations of Stark broadening parameters of Sn III lines can be found in [13,17,20]. For Sn IV, there is only one paper [21] with Stark widths and shifts for 66 spectral lines, calculated using semiempirical method of Griem [22] with atomic matrix elements obtained with the relativistic Hartree-Fock method and configuration interaction in an intermediate coupling scheme, by using the Cowan [23] approach and the COWAN code.…”

Energy-level structure ofSn3+ions

“…Emission of light by neutral tin atoms and lowly charged tin ions, Sn i -Sn v, is abundant in a wide variety of plasmas, ranging from laser-produced extremeultraviolet (EUV) light generating Sn plasma for nanolithography [1,2], divertor plasma when using tin containing materials in future thermonuclear fusion reactors [3][4][5], discharge plasma between tin whiskers causing short-circuits [6], to astrophysical environments [7][8][9][10][11][12][13][14][15]. Spectroscopic investigations on these kinds of plasmas can help characterize plasma parameters [16][17][18][19][20][21][22] such as ion and electron densities and temperatures by studying the observed line strengths and their shapes.…”