Carbon, nitrogen, and oxygen abundances in main-sequence stars. II 20 F and G stars

Clegg, R. E. S.; Lambert, David L.; Tomkin, J.

doi:10.1086/159371

Cited by 168 publications

(99 citation statements)

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“…We can see that it displays light element abudance ratios that are similar to those of CH stars already analyzed (Vanture 1992b) despite the scatter seen for such stars. Clegg et al 1981;Tomkin & Lambert 1984;Carbon et al 1987). However, as a star becomes giant, due to deepening of its convective envelope, nuclear processed material is brought from the interior to the outer layers of the star changing the surface composition.…”

Section: The Log C/n -Log O/n Diagrammentioning

confidence: 99%

High-resolution spectroscopic observations of two chemically peculiar metal-poor stars: HD 10613 and BD+04°2466

Pereira

Драке²

2009

A&A

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Aims. We determined the atmospheric parameters and abundance pattern of two chemically peculiar metal-poor stars: HD 10613 and BD+04 • 2466 in order to better understand their evolutionary state and the nature of the s-element enhancement of these stars. Methods. We used high resolution optical spectroscopy. Atmospheric parameters and abundances were determined in the localthermodynamic-equilibrium model atmospheres of Kurucz using the spectral analysis code MOOG. • 2466 the abundance of lead is in agreement with predictions from AGB models. Due to the low luminosity of these two stars, their observed s-process overabundance is better explained by mass-transfer in the past from an AGB star.

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Section: The Log C/n -Log O/n Diagrammentioning

confidence: 99%

High-resolution spectroscopic observations of two chemically peculiar metal-poor stars: HD 10613 and BD+04°2466

Pereira

Драке²

2009

A&A

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“…Let f be an unknown true value of log (Fe/H), and let E be a generally nonzero systematic error in f which results from 166, Branch & Bell (1971); 565, Balachandran (1990); 624, Edvardsson et al (1993);, Raff (19762003, Nissen (19812004, Clegg et al (19812055, Fuhrmann (19982072, Chen et al (2000. In the catalog, a complete list of numbers and references appears in a supplementary list.…”

Section: Appendix A: Zero-point Procedures For [Fe/h] Analysismentioning

confidence: 99%

Statistical cataloging of archival data for luminosity class IV–V stars

Taylor

2003

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Abstract. This paper describes the derivation of an updated statistical catalog of metallicities. The stars for which those metallicities apply are of spectral types F, G, and K, and are on or near the main sequence. The input data for the catalog are values of [Fe/H] published before 2002 February and derived from lines of weak and moderate strength. The analyses used to derive the data have been based on one-dimensional LTE model atmospheres. Initial adjustments which are applied to the data include corrections to a uniform temperature scale which is given in a companion paper (see Taylor 2003). After correction, the data are subjected to a statistical analysis. For each of 941 stars considered, the results of that analysis include a mean value of [Fe/H], an rms error, an associated number of degrees of freedom, and one or more identification numbers for source papers. The catalog of these results supersedes an earlier version given by Taylor (1994b).

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“…Unfortunately, sulphur has been ignored for many years probably due to the lack of measurable lines in the optical spectra. Presently, our knowledge of sulphur abundances is limited to only a few studies: Clegg et al (1981), François (1987François ( , 1988 and recent works by and Takada-Hidai et al (2002). Again, the disagreement on the [S/Fe] ratio at low metallicities appears: François (1987François ( , 1988 suggested the [S/Fe] ratio to be constant for stars with −1.6 < [Fe/H] < −1.0, while In the present work, we investigate the behaviour of sulphur in disk stars and the nucleosynthesis origin of this element.…”

Section: Introductionmentioning

confidence: 99%

“…Again, the disagreement on the [S/Fe] ratio at low metallicities appears: François (1987François ( , 1988 suggested the [S/Fe] ratio to be constant for stars with −1.6 < [Fe/H] < −1.0, while In the present work, we investigate the behaviour of sulphur in disk stars and the nucleosynthesis origin of this element. The investigation takes benefit of more accurate observations of sulphur lines, better determinations of stellar parameters, improved atmospheric models, and hence more reliable derivations of sulphur, silicon and iron abundances than in previous works (Clegg et al 1981;François 1987François , 1988, where the scatter of [S/Fe] for disk stars is so large that it is not clear if sulphur really behaves as an α-capture elements or not. In a following paper (Nissen et al 2002), the study will be extented to halo stars such that the trend of [S/Fe] will be covered for the whole metallicity range of −3.0 < [Fe/H] < +0.2.…”

Section: Introductionmentioning

confidence: 99%