Determination of radiative lifetimes of neutral sulfur by time-resolved vacuum-ultraviolet laser spectroscopy

Berzinsh, U.; Caiyan, Luo; Zerne, R; Svanberg, Sune; Biémont, Émile

doi:10.1103/physreva.55.1836

Cited by 34 publications

(40 citation statements)

References 27 publications

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“…With the gf -values of Berzinsh et al (1997) we find log ǫ P = 5.36 ± 0.04. From the line list used by Lambert & Luck (1978), we removed several S i lines with profiles that indicate blends.…”

Section: Sodium To Calciummentioning

confidence: 76%

The solar chemical composition

2006

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Abstract.We review our current knowledge of the solar chemical composition as determined from photospheric absorption lines. In particular we describe the recent significant revisions of the solar abundances as a result of the application of a time-dependent, 3D hydrodynamical model of the solar atmosphere instead of 1D hydrostatic models. This has decreased the metal content in the solar convection zone by almost a factor of two compared with the widely used compilation by Anders & Grevesse (1989). While resolving a number of longstandings problems, the new 3D-based element abundances also pose serious challenges, most notably for helioseismology.

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Section: Sodium To Calciummentioning

confidence: 76%

The solar chemical composition

2006

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“…Table 2. Atmospheric Parameters and Abundances Atomic line data for the phosphorus transitions shown in Table 3, was obtained from Berzinsh et al (1997) and is identical to that used in . Atomic line data for a feature Si I was taken from the Kurucz database 2 .…”

Section: Abundance Analysismentioning

confidence: 99%

Phosphorus Abundances in FGK Stars

Maas

Pilachowski

Cescutti

2017

ApJ

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We measured phosphorus abundances in 22 FGK dwarfs and giants that span -0.55 < [Fe/H] < 0.2 using spectra obtained with the Phoenix high resolution infrared spectrometer on the Kitt Peak National Observatory Mayall 4m telescope, the Gemini South Telescope, and the Arcturus spectral atlas. We fit synthetic spectra to the P I feature at 10581Å to determine abundances for our sample. Our results are consistent with previously measured phosphorus abundances; the average [P/Fe] ratio measured in [Fe/H] bins of 0.2 dex for our stars are within ∼ 1 σ compared to averages from other IR phosphorus studies. Our study provides more evidence that models of chemical evolution using the results of theoretical yields are under producing phosphorus compared to the observed abundances. Our data better fit a chemical evolution model with phosphorus yields increased by a factor of 2.75 compared to models with unadjusted yields. We also found average [P/Si] = 0.02 ± 0.07 and [P/S] = 0.15 ± 0.15 for our sample, showing no significant deviations from the solar ratios for [P/Si] and [P/S] ratios.

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“…During the past few years, time-resolved laser spectroscopy has been used extensively at the LLC and has been able to provide the astrophysicists with many new and accurate radiative lifetimes and transition probabilities (Berzinsh et al 1997a,b, Biémont et al 1998a,b, 1999. The radiative lifetime measurements in La III have been performed using that technique.…”

Section: Lifetime Measurementsmentioning

confidence: 99%

Radiative lifetimes in La III and oscillator strengths in La III and Lu III

Biémont

Li²,

Palmeri

et al. 1999

J. Phys. B: At. Mol. Opt. Phys.

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Abstract. New radiative lifetime measurements performed with time-resolved laser spectroscopy for the 6p 1/2 and 6p 3/2 levels of La III provide a unique opportunity for testing the adequacy of the relativistic Hartree-Fock approach for atomic structure calculations in this ion. As a consequence of the comparison, an extensive set of accurate f -values is provided for many La III and Lu III UV and visible transitions of astrophysical interest.

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Determination of radiative lifetimes of neutral sulfur by time-resolved vacuum-ultraviolet laser spectroscopy

Cited by 34 publications

References 27 publications

The solar chemical composition

The solar chemical composition

Phosphorus Abundances in FGK Stars

Radiative lifetimes in La III and oscillator strengths in La III and Lu III

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