Volume 369, Number 3, April III 2001
|Page(s)||1009 - 1026|
|Section||Stellar structure and evolution|
|Published online||15 April 2001|
Non-LTE line formation for MgI/II: Abundances and stellar parameters*
Model atom and first results on A-type stars
Universitäts-Sternwarte München, Scheinerstraße 1, 81679 München, Germany
2 Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Straße 1, 85740 Garching bei München, Germany
Corresponding author: N. Przybilla, email@example.com
Accepted: 11 January 2001
An extensive model atom for non-LTE line-formation calculations for neutral and singly-ionized magnesium is presented, taking into account recent improvements in the atomic data. As a test and first application of the model, stellar parameters and magnesium abundances are determined on the basis of line-blanketed LTE model atmospheres for three stars: Vega (A0 V), η Leo (A0 Ib) and HD 92207 (A0 Iae) using high and high resolution spectra at visual and near-IR wavelengths. The ionization equilibrium of Mgi/ii proves to be a sensible temperature indicator for early A-type stars at all luminosities. Evidence is given that in late A and early F-type supergiants ( K) the determination of accurate stellar parameters is hampered by the presence of a pressure inversion region in the model atmospheres at line-formation depths. The Mgi/ii lines in the observations are reproduced simultaneously by the calculated line profiles with high accuracy. For Vega spectral synthesis in the UV region of the Mgi/ii resonance lines also proves excellent consistency with the results from the visual. The dependence of the non-LTE effects on the atmospheric parameters is discussed with special emphasis on the supergiants where a strong radiation field at low particle densities favours deviations from LTE, especially in the minor ionic species of neutral magnesium. Non-LTE corrections turn out to be small in Mgi -typically 0.3 dex -even in supergiants, but are essential for an accurate effective temperature determination. From the Mgii spectrum, only the features at 4481 and 7877-96 Å react sensitively to non-LTE effects. Furthermore, the influence of microturbulence on the statistical-equilibrium calculations is investigated. The line strengths are found to be systematically affected.
Key words: atomic data / line: formation / stars: abundan ces, fundamental parameters, supergiants
© ESO, 2001
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