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Abundance and stratification analysis of the chemically peculiar star HD 103498
Uppsala University, Disciplinary Domain of Science and Technology, Physics, Department of Physics and Astronomy, Observational Astronomy.
2011 (English)In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 417, no 1, 444-452 p.Article in journal (Refereed) Published
Abstract [en]

The slow rotation and the absence of strong mixing processes in the atmospheres of chemically peculiar stars develop the ideal conditions for the appearance of abundance anomalies through the mechanism of microscopic particle diffusion. This makes these objects look spectroscopically and photometrically different from their 'normal' analogues. As a result, it is often difficult to accurately determine the atmospheric parameters of these stars, and special methods are needed for a consistent analysis of their atmospheres. The main aim of the present paper is to analyse atmospheric abundance and stratification of chemical elements in the atmosphere of the chemically peculiar star HD 103498. We find that there are two model atmospheres, computed with individual and stratified abundances, that provide a reasonable fit to the observed spectroscopic and photometric indicators: T(eff) = 9300 K, log g = 3.5 and T(eff) = 9500 K, log g = 3.6. It is shown that Mg has a large abundance gradient in the star's atmosphere with accumulation of Mg ions in the uppermost atmospheric layers, whereas Si demonstrates the opposite behaviour with accumulation in deep layers. In addition, a detailed non-local thermodynamic equilibrium (non-LTE) analysis showed that none of the Mg transitions under consideration is a subject of noticeable non-LTE effects. By comparing the photometry observations after transforming them to physical units, we estimated the radius of HD103498 to be between R = (4.56 +/- 0.77) R(circle dot) for T(eff) = 9300 K, log g = 3.5, and R = (4.39 +/- 0.75) R(circle dot) for T(eff) = 9500 K, log g = 3.6 models, respectively. We note that the lack of suitable observations in absolute units prevents us from uniquely determining the T(eff) of the star at the current stage of analysis.

Place, publisher, year, edition, pages
2011. Vol. 417, no 1, 444-452 p.
Keyword [en]
stars: atmospheres, stars: chemically peculiar, stars: fundamental parameters, stars: individual: HD 103498
National Category
Astronomy, Astrophysics and Cosmology
URN: urn:nbn:se:uu:diva-161946DOI: 10.1111/j.1365-2966.2011.19281.xISI: 000296276300052OAI: oai:DiVA.org:uu-161946DiVA: diva2:458149
Available from: 2011-11-21 Created: 2011-11-21 Last updated: 2012-10-18Bibliographically approved

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