Oscillator strengths for Zr I and Zr II and a new determination of the solar abundance of zirconium

Biémont, Émile; Grevesse, N.; Hannaford, Peter; Löwe, R. M.

doi:10.1086/159213

Cited by 179 publications

(134 citation statements)

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“…In fact NLTE effects, even on weak unsaturated Zr I lines, have been found by Brown et al (1983) for G and K giants. However, both Biemont et al (1981) and Bogdanovich et al (1996) analysed in LTE Zr I lines (34 and 21 lines, respectively) and Zr II lines (24 and 15 lines, respectively) in the solar photosphere, and found an excellent agreement between the abundances derived from both ionisation stages. Very recently Velichko et al (2010) performed a NLTE analysis of zirconium in the case of the Sun and late type stars.…”

Section: Introductionmentioning

confidence: 76%

“…Biemont et al (1981) selected lines that lie at λ < 800 nm. They derived log gf using the technique developed by , suitable for highly refractory elements like Zr, to determine lifetimes of 34 levels of Zr I and 20 levels of Zr II.…”

Section: Lines and Atomic Datamentioning

confidence: 99%

“…Bogdanovich et al (1996) computed and used log gf values for 21 Zr I lines. They give new log gf values for 15 Zr II lines among those selected by Biemont et al (1981). Their log gf are given in Table 2.…”

Section: Lines and Atomic Datamentioning

confidence: 99%

“…Only the line at 784.9 nm is retained in Table 1, as it was by Biemont et al (1981) and Vanture & Wallerstein (2002).…”

Section: Lines and Atomic Datamentioning

confidence: 99%

“…The line identifications by Moore et al (1966) on the Utrecht solar atlas have been used by Biemont et al (1981) to select 31 Zr II lines, seven of which were later discarded because the derived abundance exceeded the mean by more than 3σ, so they are likely blended with other unknown species. Gratton & Sneden (1994) used the same line list as Biemont et al (1981).…”

Section: Lines and Atomic Datamentioning

confidence: 99%

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The solar photospheric abundance of zirconium

et al. 2011

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Zirconium (Zr), together with strontium and yttrium, is an important element in the understanding of the Galactic nucleosynthesis. In fact, the triad Sr-Y-Zr constitutes the first peak of s-process elements. Despite its general relevance not many studies of the solar abundance of Zr were conducted. We derive the zirconium abundance in the solar photosphere with the same CO 5 BOLD hydrodynamical model of the solar atmosphere that we previously used to investigate the abundances of C-N-O. We review the zirconium lines available in the observed solar spectra and select a sample of lines to determine the zirconium abundance, considering lines of neutral and singly ionised zirconium. We apply different line profile fitting strategies for a reliable analysis of Zr lines that are blended by lines of other elements. The abundance obtained from lines of neutral zirconium is very uncertain because these lines are commonly blended and weak in the solar spectrum. However, we believe that some lines of ionised zirconium are reliable abundance indicators. Restricting the set to Zr II lines, from the CO 5 BOLD 3D model atmosphere we derive A(Zr) = 2.62 ± 0.06, where the quoted error is the RMS line-to-line scatter.

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Section: Introductionmentioning

confidence: 76%

Section: Lines and Atomic Datamentioning

confidence: 99%

Section: Lines and Atomic Datamentioning

confidence: 99%

“…Only the line at 784.9 nm is retained in Table 1, as it was by Biemont et al (1981) and Vanture & Wallerstein (2002).…”

Section: Lines and Atomic Datamentioning

confidence: 99%

Section: Lines and Atomic Datamentioning

confidence: 99%

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The solar photospheric abundance of zirconium

et al. 2011

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Elemental abundance analyses with DAO spectrograms: XXXI. The early F supergiants ν Her (F2 II) and 41 Cyg (F5 Ib‐II)

et al. 2008

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This series of high quality elemental abundance analyses of mostly Main Sequence normal and peculiar B, A, and F stars defines their properties and provides data for the comparison with analyses of somewhat similar stars and with theoretical predictions. Most use high dispersion and high S/N (≥ 200) spectrograms obtained with CCD detectors at the long camera of the 1.22-m Dominion Astrophysical Observatory telescope's coudé spectrograph. Here we expand the range of stars examined to include two relatively quiescent F supergiants. ν Her (F2 II) and 41 Cyg (F5 Ib-II) are analyzed as consistently as possible with previous studies. These LTE fine analyses use the ATLAS9 and the WIDTH9 programs of R. L. Kurucz. High signal-to-noise spectrograms and high quality atomic data were employed. The derived values of these photometrically constant stars are somewhat different with the abundances of ν Her being somewhat metal-poor and those of 41 Cyg being crudely solar-like. Our analyses indicate that the basic results of Luck & Wepfer (1995) who also studied ν Her and 41 Cyg are not likely to be significantly changed by new studies of all their stars.

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Elemental abundance analyses with DAO spectrograms: XXXIII. β UMa (A0mA1 IV‐V), α Dra (A0 III), π Dra (A2 IIIs), and κ Cep (B9 III)

Adelman

Gulliver

2011

Astron Nachr

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This paper presents extended analyses of β UMa (A0mA1 IV-V), α Dra (A0 III), π Dra (A2 IIIs), and κ Cep (B9 III) which have previously been studied in this series. α Dra is a metal-poor star while κ Cep has solar abundances. Both β UMa and π Dra are Am stars. Whenever possible, more accurate and precise gf values replace older values. High S/N (200+) and high dispersion Dominion Astrophysical Observatory spectrograms to the red of previously obtained spectra supplement the observations. The derived rotational velocities are 45, 25, 26, and 23 km s −1 , respectively. These LTE fine analyses use the ATLAS9 and the WIDTH9 programs of R. L. Kurucz. The results of the extended and the previous analyses are in good agreement. Thus in the past decade a significant improvement in the system of gf values has not been achieved although for many lines there have been changes. The use of additional regions has increased the quality of some results.

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Oscillator strengths for Zr I and Zr II and a new determination of the solar abundance of zirconium

Cited by 179 publications

References 0 publications

The solar photospheric abundance of zirconium

The solar photospheric abundance of zirconium

Elemental abundance analyses with DAO spectrograms: XXXI. The early F supergiants ν Her (F2 II) and 41 Cyg (F5 Ib‐II)

Elemental abundance analyses with DAO spectrograms: XXXIII. β UMa (A0mA1 IV‐V), α Dra (A0 III), π Dra (A2 IIIs), and κ Cep (B9 III)

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