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3D model atmospheres and the solar photospheric oxygen abundance

Published online by Cambridge University Press:  01 April 2008

E. Caffau  and
H.-G. Ludwig
E. Caffau
Affiliation:
GEPI, Observatoire de Paris-Meudon; 92195 Meudon, France email: Elisabetta.Caffau@obspm.fr
H.-G. Ludwig
Affiliation:
GEPI, Observatoire de Paris-Meudon; 92195 Meudon, France email: Elisabetta.Caffau@obspm.fr CIFIST Marie Curie Excellence TeamObservatoire de Paris-Meudon, 92195 Meudon, France email: Hans.Ludwig@obspm.fr
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Abstract

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In recent years the photospheric solar oxygen abundance experienced a significant downward revision. However, a low photospheric abundance is incompatible with the value in the solar interior inferred from helioseismology. For contributing to the dispute whether the solar oxygen abundance is “high” or “low”, we re-derived its photospheric abundance independently of previous analyses. We applied 3D (CO5BOLD) as well as 1D model atmospheres. We considered standard disc-centre and disc-integrated spectral atlases, as well as newly acquired solar intensity spectra at different heliocentric angles. We determined the oxygen abundances from equivalent width and/or line profile fitting of a number of atomic lines. As preliminary result, we find an oxygen abundance in the range 8.73–8.79, encompassing the value obtained by Holweger (2001), and somewhat higher than the value obtained by Asplund et al. (2005).

Keywords

Sun: abundances – Sun: photosphere – Line: formation – hydrodynamics
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 4 , Symposium S252: The Art of Modeling Stars in the 21st Century , April 2008 , pp. 35 - 39
Copyright
Copyright © International Astronomical Union 2008

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