Abundances and possible diffusion of elements in M 67 stars

@article{Onehag2013AbundancesAP,
  title={Abundances and possible diffusion of elements in M 67 stars},
  author={Anna Onehag and Bengt Gustafsson and Andreas Korn},
  journal={Astronomy and Astrophysics},
  year={2013},
  volume={562}
}
Context. The rich open cluster M 67 is known to have a chemical composition close to solar and an age of about 3.5–4.8 Gyr. It offers an important opportunity to check and develop our understanding of the physics and the evolution of solar-type stars. Aims. We present a spectroscopic study at high resolution, R ≈ 50 000, of 14 stars located on the main sequence, at the turn-off point, and on the early subgiant branch in the cluster in order to investigate its detailed chemical composition, for… 

Chemical (in)homogeneity and atomic diffusion in the open cluster M 67

Context. The benchmark open cluster M 67 is known to have solar metallicity and an age similar to that of the Sun. It thus provides us with a great opportunity to study the properties of solar twins,

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Chemical Abundances of Main-sequence, Turnoff, Subgiant, and Red Giant Stars from APOGEE Spectra. I. Signatures of Diffusion in the Open Cluster M67

Detailed chemical abundance distributions for 14 elements are derived for eight high-probability stellar members of the solar metallicity old open cluster M67 with an age of ∼4 Gyr. The eight stars
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