Line profile measurements of (4S) 6s 5S–(4S) 6p 5P transitions of Xe III

Stark halfwidth trends along the homologous sequence of doubly ionized noble gases

“…To carry out an individual analysis of data of the Ne III to Xe III lines, it is more convenient to exclude the data sets showing a large difference compared to other results, and to calculated data. For Ar III, these results come from Platiša et al (1975), for Kr III from Ahmad et al (1998) and for Xe III from Seidel et al (2001). In this case, the dispersion of the experimental data from all authors is about ±22% for the Ne III lines, ±19% for the Ar III lines, ±6% for the Kr III and ±13% for the Xe III lines.…”

“…For each paper, we provide a list of the observed ions together with the estimate of the halfwidth experimental errors. Experimental errors from Seidel et al (2001) are taken from the results graphically presented in the paper, while information about the experimental errors in the Iriarte et al (1997) and Romeo y Bidegain et al (1998) Because similar plasma sources were used we can compare the determined Stark halfwidth values along the homologous sequence of doubly ionized noble gases. However, the experiments were performed under different plasma conditions and different diagnostic techniques were used.…”

“…8, the ratio between experimental and MSE calculated halfwidth values is shown for spectral lines of the 5 S • − 5 P multiplet. The lines for which experimental data were available for the analysis are given in Table 2 Ne III, from Ahmad et al (1998) for Kr III, and from Seidel et al (2001) for Xe III show higher ratios, between 1.4 and 1.7. It is possible to make an additional comparison between experimental and calculated results.…”

“…Owing to these similarities, a gradual increase of the spectral line halfwidths, i.e., the systematic trend should be expected in these cases. For the analysis of (n − 1)d − np and ns−np transitions, the following references are available: Platiša et al (1975), Konjević & Pittman (1987), Purić et al (1988), Kobilarov & Konjević (1990), Uzelac et al (1993), Djeniže et al (1996), Iriarte et al (1997), Romeo y Bidegain et al (1998), Ahmad et al (1998), Blagojević et al (2000), Milosavljević et al (2000Milosavljević et al ( , 2001, Seidel et al (2001), Peláez et al (2006), Bukvić et al (2008), Peláez et al (2009Peláez et al ( ),Ćirišan et al (2011 and Djurović et al (2011).…”

Stark widths of Sc IV spectral lines within 4s-4p transition array

“…Data on Stark broadening are needed for laboratory plasmas diagnostic and investigation (Konjević, 1999;Torres et al, 2006;Peláez et al, 2009), laser produced plasma analysis, modelling and diagnostics (Richou & Molitor, 1970;Gornushkin et al, 1999;Sorge et al, 2000;Seidel et al, 2001) and inertial fusion plasma (Keane et al, 1990;Griem, 1992). Stark broadening data are also useful in technology, as for example for laser welding and piercing of various metals (Dimitrijević & Sahal-Bréchot, 2014), design, investigation and improvement of effectivity of various light sources based on plasma (Wieser et al, 1997;Seidel et al, 2001), and the design and developing of lasers (Csillag & Dimitrijević, 2004;Dimitrijević & SahalBréchot, 2014). In many astrophysical plasmas Stark broadening of spectral lines is very important or at least non negligible and should be taken into account (Beauchamp et al, 1997;Popović et al, 2001;Dimitrijević, 2003;Dimitrijević & Sahal-Bréchot, 2014).…”