Stark broadening and shift of singly-ionized argon spectral lines in higher multiplets

Djeniže, S.; Malešević, Milka; Srećković, A.; Milosavljevic, M. Vranjes; Purić, J.

doi:10.1016/0022-4073(89)90011-3

Cited by 19 publications

(31 citation statements)

References 19 publications

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“…Our Stark widths calculated as described above are presented in Table 1 along with the experimental results of [18][19][20][21][22][23]. Table 1 is organized in the following way: In the first five columns of Table 1, we give the transition array, transition, wavelength, electron temperature (T) and electron density (N e ).…”

Section: Stark Widthsmentioning

confidence: 99%

“…In Figure 1, we present our electron impact Stark width as a function of temperature for the interval from 5000 to 60,000 K along with the experimental values of [18][19][20][21][22][23] for the transition ( 3 P) 3d 4 D 7/2 -( 3 P) 4p 4 D o 7/2 (λ = 4013.86 Å). All the experimental results are normalized to an electron density of 10 17 cm −3 .…”

Section: Stark Widthsmentioning

confidence: 99%

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Stark Widths of Ar II Spectral Lines in the Atmospheres of Subdwarf B Stars

Hamdi

Nessib

Dimitrijević

2017

Atoms

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Stark broadening parameters are of interest for many problems in astrophysics and laboratory plasmas investigation. Ar II spectral lines are observed in many kinds of stellar atmospheres such as the atmospheres of B-Type stars and subdwarf B stars. In this work, we present theoretical Stark widths for Ar II spectral lines. We use the impact semiclassical perturbation approach. Our results are compared with the available experimental values. Finally, the importance of the Stark broadening mechanism is studied in atmospheric conditions of subdwarf B stars.

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Section: Stark Widthsmentioning

confidence: 99%

Section: Stark Widthsmentioning

confidence: 99%

Stark Widths of Ar II Spectral Lines in the Atmospheres of Subdwarf B Stars

Hamdi

Nessib

Dimitrijević

2017

Atoms

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“…2) are taken from Popenoe & Shumaker (1965), Jalufka et al (1966), Roberts (1966), Chapelle et al (1968ab), Roberts (1968), Konjević et al (1970), Klein (1973), Labat et al (1974), Behringer & Thoma (1978), Vaessen et al (1985), Nick & Helbig (1986), Pittman & Konjević (1986), Vitel & Skowronek (1987), Abbas et al (1988), Djeniže et al (1989), Dzierzega & Musiol (1994), Pellerin et al (1997), Aparicio et al (1998) and Iglesias et al (2006).…”

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confidence: 99%

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

Peláez¹,

Djurović

Cirisan

et al. 2010

A&A

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Aims. The aim of this work is to analyse experimental Stark halfwidths behaviour for the ( 3 P)ns−( 3 P)np and ( 3 P)np−( 3 P)nd transitions along the homologous sequence of single ionized noble gases. This kind of trend analysis can be useful for Stark halfwidths predictions and therefore for spectroscopic diagnostic of astrophysical plasmas. Methods. The compilation of Stark halfwidths was done taking into account the measurements developed in the last decades. The experimental results and observed Stark halfwidth trends for different multiplets of ionized noble gases were compared with the modified semiempirical formula (MSE) calculations and other theoretical estimations.Results. The analysis shows that the halfwidths of the spectral lines in all observed multiplets belonging to the same transitions have a similar trend along the homologous sequence. Stark halfwidths of ( 3 P)ns−( 3 P)np transitions are more or less constant, while those of ( 3 P)np−( 3 P)nd transitions have a clear increasing slope. A qualitative explanation of the observed Stark halfwidth trends based on the energy level structure is also given.

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“…In Hamdi et al (2019), we have compared our Stark shifts with experimental results (Djeniže et al, 1989;Dzierzega & Musiol, 1994;Aparicio et al, 1998;Djurović et al, 2013) for Ar II spectral lines. We found good agreement with experimental results except for some transitions.…”

Section: Resultsmentioning

confidence: 99%

On the semiclassical perturbation Stark shifts of Ar II spectral lines

Hamdi¹,

Nessib²,

Sahal‐Bréchot³

et al. 2020

caosp

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We present in this paper Stark shifts as a function of temperature for 20 spectral lines of Ar II belonging to 4p -4d transition array. Calculations are made using semiclassical perturbation approach in impact approximation. Atomic data used in this calculation are carried out using Hartree-Fock method with relativistic corrections. Singly charged argon (Ar II) spectral lines are observed in many astrophysical plasmas. Ar II spectral lines are also important for laboratory plasmas and laser physics and technology.

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Stark broadening and shift of singly-ionized argon spectral lines in higher multiplets

Cited by 19 publications

References 19 publications

Stark Widths of Ar II Spectral Lines in the Atmospheres of Subdwarf B Stars

Stark Widths of Ar II Spectral Lines in the Atmospheres of Subdwarf B Stars

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

On the semiclassical perturbation Stark shifts of Ar II spectral lines

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