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The dependence of the energy distribution on the abundances of A-star atmosphere models

Published online by Cambridge University Press:  02 March 2005

J. Krtička ,
Z. Mikul´šek ,
J. Zverko  and
J. Žižňovský
J. Krtička
Affiliation:
Institute of Theoretical Physics and Astrophysics, Masaryk University, Kotlářská 2, CZ-611 37 Brno, Czech Republic email: krticka@physics.muni.cz, mikulas@dior.ics.muni.cz
Z. Mikul´šek
Affiliation:
Institute of Theoretical Physics and Astrophysics, Masaryk University, Kotlářská 2, CZ-611 37 Brno, Czech Republic email: krticka@physics.muni.cz, mikulas@dior.ics.muni.cz
J. Zverko
Affiliation:
Astronomical Institute of the Slovak Academy of Sciences, SK-059 60 Tatranská Lomnica, Slovak Republic email: zve@ta3.sk, ziga@ta3.sk
J. Žižňovský
Affiliation:
Astronomical Institute of the Slovak Academy of Sciences, SK-059 60 Tatranská Lomnica, Slovak Republic email: zve@ta3.sk, ziga@ta3.sk
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Abstract

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We calculated the energy distributions of A-star atmospheres (${{T}_\text{eff}=10 000}\,{\rm K},{\log g=4.0}$) for ranges of the abundances of silicon and other light chemical elements using adequate model atmospheres. We discuss the reasons for and the magnitudes of the calculated departures of the stellar energy distribution and uvby magnitudes from those of normal stars.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

Keywords

Radiative transferstars: atmospheresstars: chemically peculiarstars: early-type
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2004 , Issue IAUS224 , July 2004 , pp. 706 - 710
Copyright
© 2004 International Astronomical Union