Influence of Inelastic Collisions with Hydrogen Atoms on Non-LTE Oxygen Abundance Determinations

• Published in: Astronomy letters Vol. 44; no. 6; pp. 411 - 419
• Main Authors: Sitnova, T. M., Mashonkina, L. I.
• Format: Journal Article
• Language: English
• Published: Moscow Pleiades Publishing 01.06.2018; Springer Nature B.V
• Subjects: Abundance; Astronomy; Astrophysics and Astroparticles; Atmospheric models; Hydrogen; Hydrogen atoms; Inelastic collisions; Iron; Metallicity; Observations and Techniques; Oxygen; Physics; Physics and Astronomy; Stars; Stellar atmospheres; Galactic chemical evolution; solar and stellar oxygen abundances; line formation under non-LTE conditions
• ISSN: 1063-7737; 1562-6873
• DOI: 10.1134/S1063773718060063

We present the results of our modeling of the O I line formation under non-LTE conditions in the atmospheres of FG stars. The statistical equilibrium of O I has been calculated using Barklem’s quantum-mechanical rates of inelastic collisions with hydrogen atoms. We have determined the non-LTE oxygen abundance from atomic O I lines for the Sun and 46 FG stars in a wide metallicity range, −2.6 < [Fe/H] < 0.2. The application of accurate atomic data has led to an increase in the departures from LTE and a decrease in the oxygen abundance compared to the use of Drawin’s theoretical approximation. The change in the non-LTE abundance from the infrared O I 7771-5 Å triplet lines is 0.11 dex for solar atmospheric parameters and diminishes in absolute value with decreasing metallicity. We have revised the [O/Fe]–[Fe/H] relationship derived by us previously. The change in [O/Fe] is small in the [Fe/H] range from −1.5 to 0.2. For stars with [Fe/H] < −1 the [O/Fe] ratio has increased so that [O/Fe] = 0.60 at [Fe/H] = −0.8 and rises to [O/Fe] = 0.75 at [Fe/H] = −2.6.