Stark widths of doubly ionized argon spectral lines

Djeniže, S.; Bukvić, S.; Srećković, A.; Platiša, M.

doi:10.1088/0953-4075/29/3/010

Cited by 6 publications

(39 citation statements)

References 18 publications

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“…For that purpose, we used the modified semiempirical formula MSE (Dimitrijević & Konjević 1980) and the simplified modified semiempirical formula SMSE (Dimitrijević & Konjević 1987) which we discuss below. The best agreement with the calculated halfwidths for Ne III is obtained with data from Konjević & Pittman (1987), Purić et al (1988) and Uzelac et al (1993); for Ar III with data from Konjević & Pittman (1987) and Djurović et al (2011) and close results from Kobilarov & Konjević (1990) and Djeniže et al (1996); for Kr III the best agreement is obtained with data from Konjević & Pittman (1987) andĆirišan et al (2011 and, finally, for Xe III with data from Konjević & Pittman (1987) and Peláez et al (2006Peláez et al ( , 2009. Taking into account experimental errors and calculation uncertainties, the experimental and theoretical data for all Ne III, Ar III, Kr III and Xe III lines for ns − np transition agree reasonably well, if we exclude results from Iriarte et al (1997).…”

Section: Analysis Of the Stark Halfwidths For The (N − 1)d -Np And Nssupporting

confidence: 75%

“…7b, but the dispersion of the results is within ±14%. The same dispersion appears for the two data from Platiša et al (1975) for Ar III, while the results from Djeniže et al (1996) are within ±20%. The Kr III results from Milosavljević et al (2000) are within ±13%.…”

Section: Analysis Of Thesupporting

confidence: 73%

“…3) are taken from Platiša et al (1975), Konjević & Pittman (1987), Purić et al (1988), Kobilarov & Konjević (1990), Djeniže et al (1996), Bukvić et al (2008) and Djurović et al (2011). Results for Kr III (Fig.…”

Section: Analysis Of the Stark Halfwidths For The (N − 1)d -Np And Nsmentioning

confidence: 99%

“…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).…”

Section: Introductionmentioning

confidence: 99%

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

Peláez

Djurović

Cirisan

et al. 2012

A&A

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Aims. The aim of this work is to analyze the behavior of experimentally determined Stark halfwidths for (n− 1)d− np and ns − np transitions along the homologous sequence of doubly ionized noble gases. Methods. We analyzed the Stark halfwidth trends including all available experimental data. Stark halfwidth results for the above mentioned transitions and corresponding multiplets were compared with the halfwidths calculated using the modified semiempirical formula (MSE) and the simplified modified semiempirical formula (SMSE). In case of Ne III the calculation made by semiclassicalperturbation formalism (SCPF) is also presented. Results. Stark halfwidths corresponding to (n − 1)d − np and ns − np transitions have been analyzed along the homologous sequence of doubly ionized noble gases. For all multiplets observed in this work, the analysis shows that the halfwidths of the spectral lines belonging to the same transition show a similar trend along the homologous sequence. Stark halfwidths of ns − np transitions have a clearly increasing trend. On the other hand, for (n − 1)d − np transitions, there are not enough data to make a similar conclusion. This type of trend analysis can be useful for Stark halfwidth predictions and hence for spectroscopic diagnostics of astrophysical plasmas.

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Section: Analysis Of the Stark Halfwidths For The (N − 1)d -Np And Nssupporting

confidence: 75%

Section: Analysis Of Thesupporting

confidence: 73%

Section: Analysis Of the Stark Halfwidths For The (N − 1)d -Np And Nsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

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

Peláez

Djurović

Cirisan

et al. 2012

A&A

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“…Although interest in Stark width and shift of Ar iii lines exists, however, only few experimental works are devoted to the determination of these parameters (Platiša et al 1975; Dimitrijević & Konjević 1987; Konjević & Pittman 1987; Purić et al 1988; Kobilarov & Konjević 1990; Djeniže et al 1996; Bukvić et al 2008). All the above‐mentioned papers report Stark half‐width measurements and cover wavelength regions from 214 to 350 nm.…”

Section: Introductionmentioning

confidence: 99%

Stark broadening of ultraviolet Ar iii spectral lines

Djurović

Mar

Peláez

et al. 2011

Monthly Notices of the Royal Astronomical Society

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This paper presents the results of an experimental study of the Stark broadening and a shift of some double‐ionized argon spectral lines in a plasma of a low‐pressure‐pulsed arc. Electron densities of (3.5–9.0) × 1022 m−3 are determined by a two‐wavelength interferometry method and electron temperatures of 16 000–24 000 K are determined from the Boltzmann plot of 13 Ar ii spectral lines. The Stark parameter results obtained are analysed and compared with the available experimental results of other authors as well as with the calculated values obtained from modified semi‐empirical formulae. All investigated spectral lines belong to the ultraviolet spectral region. The data obtained can be of astrophysical interest.

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Stark widths of Ar III spectral lines in the atmospheres of subdwarf B stars

Hamdi¹,

Nessib²,

Sahal‐Bréchot³

et al. 2014

Advances in Space Research

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Using semiclassical perturbation approach in impact approximation, we have calculated Stark widths for 32 spectral lines of doubly charged argon (Ar III). Oscillator strengths are calculated using Hartree-Fock method with relativistic correction (HFR) and an atomic model including 17 configurations. Energy levels are taken from NIST database. For perturbing levels for which the corresponding energy does not exist in NIST database, the calculated energies are used. Our widths are compared with the experimental results. The results presented here are of interest for modelling and investigation of stellar atmospheres since argon in different ionization stages is observed in many astrophysical objects. Finally, the importance of Stark broadening mechanism is studied in the atmospheric conditions of sdB stars. Electron impact Stark widths are compared to thermal Doppler widths as a function of temperature and optical depth of atmospheric layers.

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Stark widths of doubly ionized argon spectral lines

Cited by 6 publications

References 18 publications

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

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

Stark broadening of ultraviolet Ar iii spectral lines

Stark widths of Ar III spectral lines in the atmospheres of subdwarf B stars

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