EPJ Web of Conferences
Volume 19, 2012Assembling the Puzzle of the Milky Way
|Number of page(s)||2|
|Section||How Stars and Interstellar Medium interplay? ISM Large Scale Structure, Stellar Formation, Gas Infall, Galactic Fountains, . . .|
|Published online||07 February 2012|
Chemical homogeneity in the Orion Association: Oxygen abundances of B stars
1 Observatorio Nacional, Rio de Janeiro, Brazil
2 University of Arizona, Steward Observatory, USA
3 University of Maryland, USA
a e-mail: firstname.lastname@example.org
We present non-LTE oxygen abundances for a sample of B stars in the Orion association. The abundance calculations included non-LTE line formation and used fully blanketed non-LTE model atmospheres. The stellar parameters were the same as adopted in the previous study by Cunha & Lambert (1994). We find that the young Orion stars in this sample of 10 stars are described by a single oxygen abundance with an average value of A(O) = 8.78 and a small dispersion of ±0.05, dex which is of the order of the uncertainties in the analysis. This average oxygen abundance compares well with the average oxygen abundance obtained previously in Cunha & Lambert (1994): A(O) = 8.72 ± 0.13 although this earlier study, based upon non-blanketed model atmospheres in LTE, displayed larger scatter. Small scatter of chemical abundances in Orion B stars had also been found in our previous studies for neon and argon; all based on the same effective temperature scale. The derived oxygen abundance distribution for the Orion association compares well with other results for the oxygen abundance in the solar neighborhood.
© Owned by the authors, published by EDP Sciences, 2012
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