Influence of Inelastic Collisions with Hydrogen Atoms on Non-LTE Oxygen Abundance Determinations
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...
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Published in | Astronomy letters Vol. 44; no. 6; pp. 411 - 419 |
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Language | English |
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01.06.2018
Springer Nature B.V |
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Abstract | 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. |
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AbstractList | 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. |
Author | Sitnova, T. M. Mashonkina, L. I. |
Author_xml | – sequence: 1 givenname: T. M. surname: Sitnova fullname: Sitnova, T. M. email: sitnova@inasan.ru organization: Institute of Astronomy, Russian Academy of Sciences, Herzen State Pedagogical University – sequence: 2 givenname: L. I. surname: Mashonkina fullname: Mashonkina, L. I. organization: Institute of Astronomy, Russian Academy of Sciences |
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CitedBy_id | crossref_primary_10_1134_S1063773723050018 crossref_primary_10_1093_mnras_stz2484 crossref_primary_10_1093_mnrasl_slac015 crossref_primary_10_1051_0004_6361_202141740 crossref_primary_10_1093_mnras_stac1675 crossref_primary_10_1051_0004_6361_202038805 crossref_primary_10_1134_S1063772919090063 crossref_primary_10_1038_s41550_021_01544_4 crossref_primary_10_1093_mnras_stab786 crossref_primary_10_1093_mnras_stz1511 crossref_primary_10_1093_mnras_stab2160 |
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Snippet | 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... |
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SubjectTerms | 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 |
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