Profiles of the He i 23P-33D line at high densities

Büscher, S.; Glenzer, S. H.; Wrubel, Th.; Kunze, H.‐J.

doi:10.1016/0022-4073(95)00042-j

Cited by 15 publications

(22 citation statements)

References 20 publications

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“…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). 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.…”

Section: Resultsmentioning

confidence: 97%

“…Ratios of the experimental total Stark FWHM (W exp t ) to the various theoretical (W th t ) predictions vs. electron temperature for λ = 587.56 nm. , ♦, ∇, , and represent our experimental data and those from Büscher et al (1995), Kobilarov et al (1989), Berg et al (1962), Kelleher (1981), and Purić et al (1970), 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.…”

Section: Resultsmentioning

confidence: 99%

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

Milosavljević

Djeniže

2002

New Astronomy

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Section: Resultsmentioning

confidence: 97%

Section: Resultsmentioning

confidence: 99%

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

Milosavljević

Djeniže

2002

New Astronomy

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“…For the comparison, we used theoretical (Griem 1974;Bassalo et al 1982;Sahal-Bréchot et al 2013) and experimental data (Wulff 1958;Berg et al 1962;Bötticher et al 1963;Lincke 1964;Greig & Jones 1970;Kusch 1971; Vujičić et al 1989;Kobilarov et al 1989;Pérez et al 1991Pérez et al , 1995Büscher et al 1995;Djeniže et al 1995;Mijatović et al 1995;Milosavljević & Djeniže 2002a,b, 2003Pérez et al 2003;Gao et al 2008). The experimental data were obtained form various plasma sources with different plasma conditions and with different plasma diagnostic methods.…”

Section: Comparison With Other Resultsmentioning

confidence: 99%

Stark broadening of lines from transition between statesn = 3 ton = 2 in neutral helium

Djurović

Savić

et al. 2014

A&A

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Context. The Stark broadening of the spectral lines of the wavelengths 501. 6, 667.8, 728.1, 388.9, 587.6, and 706.5 nm from neutral helium in plasmas are studied theoretically and experimentally. Aims. The aim of this work is to provide information about the connection between the shape and width of spectral lines and the electron density and temperature to be used as a diagnostic tool. Methods. The theoretical calculations were carried out through molecular dynamics computer simulations with noninteracting particles. The experimental measurements were done in a plasma of pure helium generated in an electromagnetically driven T-tube. The plasma diagnostics used previous results about the Stark broadening of the He I 447.1 nm and He I 492.2 nm lines and the coherence between the shape of these spectra and those obtained here. The electron temperature was obtained through a Boltzmann-plot of eight lines of Si II. Results. Several tables of width and shift are provided in a wide range of electron density and temperature. Furthermore, we supply several fitting formulas, which allow calculating the plasma electron density from the measured values of the spectral line widths. The results obtained in the laboratory and in the simulations are compared with the data from the literature.

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“…The cases of the 6678 Å (2 1 P • −3 1 D) and 5876 Å (2 3 P • −3 3 D) HeI visible lines are chosen by considering the same conditions of densities N e and temperatures T as the experiments of Gauthier et al (1981) and Bücher et al (1995), and an upper cut-off at R D for the Coulomb Debye model and at R c for the Cut-off and the Ion Sphere models.…”

Section: Introductionmentioning

confidence: 99%

Semi-classical Stark broadening calculations of HeI lines in a non-ideal plasma

Chaouacha¹,

Sahal‐Bréchot²,

Nessib³

2007

A&A

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New semi-classical collision functions are used to compute the inelastic contribution to the impact electronic total width, by considering three interaction potentials (Coulomb Debye, Cut-off, and Ion Sphere). Numerical results are calculated for the neutral helium 6678 Å (2 1 P • −3 1 D) and 5876 Å (2 3 P • −3 3 D) visible lines. The lines corresponding to these transitions are isolated, and the plasma is weakly non-ideal for all temperatures and electronic densities of interest. For electronic collisions, semi-classical perturbation theory is sufficient and the impact approximation is well satisfied. The ion effects can be treated within the quasistatic approximation, and the quasistatic ionic contribution is dominated by the polarization (or quadratic) r −4 p -interaction. To consider both the electron and the ion effects, the microfield distributions and the complete reduced Stark profile of isolated line are calculated using different methods. The computed total widths corresponding to the three interaction potentials are compared to the available experimental widths and then approximated by appropriate formulae. The data we obtained provide an opportunity to test various approximations included in the semi-classical perturbation formalism. They are also of interest for stellar spectroscopic diagnosis in dense atmospheres (white dwarfs for instance).

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Profiles of the He i 23P-33D line at high densities

Cited by 15 publications

References 20 publications

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

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

Stark broadening of lines from transition between statesn = 3 ton = 2 in neutral helium

Semi-classical Stark broadening calculations of HeI lines in a non-ideal plasma

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