Convergent calculations for electron impact broadening and shift of neutral helium lines

Ion contribution to the astrophysical important 388.86, 471.32 and 501.56 nm He I spectral lines broadening

“…The W G t (Griem 1974) and W BCW t (Bassalo et al 1982) values are calculated using Eq. (226) from Griem (1974) with the W e and A values predicted by the G (Griem 1974) and BCW (Bassalo et al 1982) Freudenstein & Cooper (1978) and Dimitrijević & Konjević (1986), for the 667.82 nm line, exceed all other W e data presented in Table 2.…”

“…3). Theoretical W t values presented by Bassalo et al (1982) in pm within ±12% accuracy), static ion broadening parameter (A exp , dimensionless within ±15% accuracy) and ion dynamic coefficient (D exp , dimensionless within ±20% accuracy) at a given electron temperature (T in 10 3 K) and electron density (N in 10 22 m −3 ). Ref presents the values given in this work (Tw) and those used from other authors: K, Kelleher (1981); B, Berg et al (1962); KK, Kobilarov et al (1989); RS, Roder & Stampa (1964); PL, Purić et al (1970); BG, Büscher et al (1995); P, Pérez et al (1991); M, Mijatović et al (1995); Ga, Gauthier et al (1981); VK, Vujičić & Kobilarov (1988).…”

“…Ref presents the values given in this work (Tw) and those used from other authors: K, Kelleher (1981); B, Berg et al (1962); KK, Kobilarov et al (1989); RS, Roder & Stampa (1964); PL, Purić et al (1970); BG, Büscher et al (1995); P, Pérez et al (1991); M, Mijatović et al (1995); Ga, Gauthier et al (1981); VK, Vujičić & Kobilarov (1988). The index G, BCW and DSB denote theoretical data taken from Griem (1974), Bassalo et al (1982) and Dimitrijević & Sahal-Bréchot (1990), respectively at a given T and N. 3%-18% with the best agreement for the 447.15 nm line (see Fig. 4).…”

“…, ♦, ∇, , and represent our experimental data and those from Gauthier et al (1981), Mijatović et al (1995), Pérez et al (1991), Kelleher (1981), and Vujičić & Kobilarov (1988), respectively. Filled, empty and half divided symbols represent the ratios related to the theories taken from Griem (1974), Bassalo et al (1982) and Dimitrijević & Sahal-Bréchot (1990), respectively.…”

“…The T -values used are typical for many cosmic light sources. Using a deconvolution procedure described by Milosavljević & Poparić (2001) we have obtained, for the first time, on the basis of the observed line profile asymmetry, the ion contribution to the line shape from the quasistatic ion (parameter A) and ion dynamic effect (coefficient D) (Griem 1974;Barnard et al 1974;Bassalo et al 1982) and, also, the separate electron (W e ) and ion (W i ) contributions to the total Stark width (W t ). As a plasma source we have used a linear, low-pressure, pulsed arc operated in five various discharge conditions.…”