Oxygen abundances in nearby stars - Clues to the formation and evolution of the Galactic disk
By I. Ramírez, C. Allende Prieto, D. Lambert. 2007
170 citations recorded by the source corpus.
The abundances of iron and oxygen are homogeneously determined in a sample of 523 nearby (d 5500 K and [Fe/H] −0.3, we find no obvious indication of a sudden decrease (i.e., a “knee”) in the [O/Fe] vs. [Fe/H] pattern of thick-disk stars that would connect the thick and thin disk trends at a high metallicity. We conclude that Type Ia supernovae (SN Ia) did not contribute significantly to the chemical enrichment of the thick disk. In the −0.8 < [Fe/H] < +0.3 range, thin-disk stars show decreasing [O/Fe] ratios from about 0.4 to 0.0 that require a SN Ia contribution. The implications of these results for studies of the formation and evolution of the Galactic disk are discussed.
Subfields: Astronomy and Astrophysics
View Paper: https://www.semanticscholar.org/paper/e22b8890cd04a5668f17f93519063c58d890d5e3
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In Astronomy and Astrophysics
Citations in the corpus
- Gaia FGK benchmark stars: Effective temperatures and surface gravities (2015, methodology): “Ten or more Gaia FGK benchmark stars were analysed spectroscopically by Valenti & Fischer (2005), Luck & Heiter (2005), and Bruntt et al. (2010), while the parallax method was applied for more than ten stars by Allende Prieto et al. (2004) and Ramírez et al. (2007).”
- Gaia FGK benchmark stars: Metallicity (2013, background): “…which have different spatial velocities (e.g. Soubiran 1993; Article number, page 1 of 27 Soubiran et al. 2003), different chemical abundance patterns (Bensby et al. 2004; Ramírez et al. 2007) and ages (for example the works of Fuhrmann 1998; Allende Prieto et al. 2006), than the thin disk stars.”
- Evolution of interstellar dust and stardust in the solar neighbourhood (2007, background): “…seems not to have played a mayor role during most of the lifetime of the Milky Way, except for the very first evolutionary phase for which stellar dynamics (cf. Helmi et al. 2006) and elemental abundances (Reddy et al. 2006; Ramírez et al. 2007) indicate that there were major merging events.”