Mg II 448.1 nm Spectral Line Stark Broadening Parameters

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

doi:10.1143/jjap.44.1450

Cited by 7 publications

(5 citation statements)

References 15 publications

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“…Theoretical Stark broadening line widths (in pm) are displayed in the fifth column and, where appropriate, the experimental values from the literature. The final column displays the theoretical Stark line shift (a positive shift is red) and in the same way the experimental values of other authors: see Cappelle & Sahal-Bréchot (1970), Jones et al (1972), Fleurier et al (1977, Goldbach et al (1982), Bukvić et al (2004), Djeniže et al (2004), Djeniže et al (2005) and Cvejić et al (2013). Our Stark full width at half-maximum (FWHM) values are in good agreement with the experimental ones, with some exceptions.…”

Section: Stark Width Fwhm and Stark Line Shiftsupporting

confidence: 87%

“…In the same way, have measured resonance h and k spectral lines and values of the 2790.77-and 2797.99-Å lines in the 3p-3d transition. Djeniže, Srećković & Bukvić (2005) have again measured the Stark width and shift of the 4481.13-Å spectral line in the 3d 2 D 5/2 -4f 2 F 0 7/2 transition in nitrogen plasma generated in an optically thin linear, low-pressure, pulsed arc discharge. The Stark broadening parameter of the same line was also measured by Cvejić et al (2013) with a laser-induced plasma.…”

Section: Introductionmentioning

confidence: 99%

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Theoretical transition probabilities, radiative lifetimes and Stark broadening parameters of singly ionized magnesium

Moreno-Díaz

Alonso‐Medina

2019

Monthly Notices of the Royal Astronomical Society

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The presence of spectral lines of singly ionized magnesium (Mg ii) in stellar atmospheres has been reported in different stars. Recently, the low-resolution spectrum obtained from Supernova 2014 J in M82, in which Mg ii absorption lines centred on 4400 Å as well as 7600 Å stand out, has been analysed. This is the motive for the atomic data calculations in this work, which are of much interest in the astrophysical area. In this article, ab initio relativistic Hartree–Fock calculations in an intermediate coupling formalism using Cowan’s code allowed us to obtain the required transition probabilities to calculate the theoretical radiative lifetimes for excited nS−, nP−, nD− and nF− states of singly ionized magnesium. An asymptotic dependence of lifetime (τnl) on the effective principal quantum number (n*) has been determined. Also, the Griem semi-empirical approach was used to obtain the theoretical Stark parameters (width and shift) of spectral lines; these data are displayed for an electron density of 1017 cm−3 and temperatures T = 10–100 (×103 K). We have compared the results of lifetimes for 16 levels and Stark parameters for seven spectral lines with previously reported experiments available in the literature. Finally, we discuss the behaviour of the Stark parameters versus temperature for three relevant spectral lines (2802.70, 2797.99 and 7868.04 Å).

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Section: Stark Width Fwhm and Stark Line Shiftsupporting

confidence: 87%

Section: Introductionmentioning

confidence: 99%

Theoretical transition probabilities, radiative lifetimes and Stark broadening parameters of singly ionized magnesium

Moreno-Díaz

Alonso‐Medina

2019

Monthly Notices of the Royal Astronomical Society

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“… c Measured at n e = 1.35 × 10 17 cm −3 and T = 16.9 × 10 3 K (Djeniže, Srećković & Bukvić 2005; Lesage 2009). …”

Section: Analysis and Discussionmentioning

confidence: 99%

“…Estimated using the classical formula and n eff = 4 Dimitrijević & Sahal-Bréchot (1995). calculated at n e = 1.35 × 10 17 cm −3 and T = 16.9 × 10 3 K. Measured at n e = 1.35 × 10 17 cm −3 and T = 16.9 × 10 3 K(Djeniže, Srećković & Bukvić 2005;Lesage 2009).…”

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confidence: 99%

Pressure shifts and abundance gradients in the atmosphere of the DAZ white dwarf GALEX J193156.8+011745★

Vennes¹,

Kawka²,

Németh³

2011

Monthly Notices of the Royal Astronomical Society

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We present a detailed model atmosphere analysis of high‐dispersion and high signal‐to‐noise ratio spectra of the heavily polluted DAZ white dwarf GALEX J1931+0117. The spectra obtained with the Very Large Telescope (VLT)‐Kueyen/UV‐Visual Echelle Spectrograph show several well‐resolved Si ii spectral lines enabling a study of pressure effects on line profiles. We observed large Stark shifts in silicon lines in agreement with theoretical predictions and laboratory measurements. Taking into account Stark shifts in the calculation of synthetic spectra, we reduced the scatter in individual line radial velocity measurements from ∼3 to ≲1 km s−1. We present revised abundances of O, Mg, Si, Ca and Fe based on a critical review of line‐broadening parameters and oscillator strengths. The new measurements are generally in agreement with our previous analysis with the exception of magnesium with a revised abundance of a factor of 2 lower than previously estimated. The magnesium, silicon and iron abundances exceed solar abundances, but the oxygen and calcium abundances are below solar. Also, we compared the observed line profiles to synthetic spectra computed with variable accretion rates and vertical abundance distributions assuming diffusive steady state. The inferred accretion rates vary from for calcium to 2 × 109 g s−1 for oxygen. We find that the accretion flow must be oxygen rich while being deficient in calcium relative to solar abundances. The lack of radial velocity variations between two measurement epochs suggests that GALEX J1931+0117 is probably not in a close binary and that the source of the accreted material resides in a debris disc.

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“…Broadening parameters have been determined theoretically for: Ar ii 476.5 nm, 480.6 nm and Kr ii 469.4 nm lines (Dimitrijević & Csillag 2006), Cd i 33 singlets and 37 triplets (Simić et al 2005a), 26 Ne v multiplets (Hamdi et al 2007) and 15 Si VI multiplets (Hamdi et al 2008). Broadening parameters have been obtained experimentally for: C i 247.8561 nm (Djeniže et al 2006b), Mg ii 448.1 nm (Djeniže et al 2005b), Fe i 381.58 nm (Bengoechea et al 2006) and Fe i 538.34 nm (Bengoechea et al 2005) Stehlé et al (2005) have examined current Stark broadening theory as a basis for diagnostics of low-temperature plasmas and Mahmoudi et al (2008) have provided new expressions for diagonal multiplet factors of complex configurations, required for studies of isolated lines. Zmerli et al (2008) have proposed an improved interpolation method for widths as a function of temperature.…”

Section: Isolated Linesmentioning

confidence: 97%

Division Xii / Commission 14 / Working Group Collision Processes

Peach¹,

Dimitrijević²,

Stancil³

2008

Proc. IAU

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Research in atomic and molecular collision processes and spectral line broadening has been very active since our last report (Schultz & Stancil 2007, Allard & Peach 2007). Given the large volume of the published literature and the limited space available, we have attempted to identify work most relevant to astrophysics. Since our report is not comprehensive, additional publications can be found in the databases at the web addresses listed in the final section. Elastic and inelastic collisions among electrons, atoms, ions, and molecules are included and reactive processes are also considered, but except for charge exchange, they receive only sparse coverage.

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Mg II 448.1 nm Spectral Line Stark Broadening Parameters

Cited by 7 publications

References 15 publications

Theoretical transition probabilities, radiative lifetimes and Stark broadening parameters of singly ionized magnesium

Theoretical transition probabilities, radiative lifetimes and Stark broadening parameters of singly ionized magnesium

Pressure shifts and abundance gradients in the atmosphere of the DAZ white dwarf GALEX J193156.8+011745★

Division Xii / Commission 14 / Working Group Collision Processes

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