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Modeling: connecting interior and atmosphere

Published online by Cambridge University Press:  19 December 2013

A. Hui-Bon-Hoa
A. Hui-Bon-Hoa*
Affiliation:
Université de Toulouse, UPS-OMP, IRAP, Toulouse, France CNRS, IRAP, 14 avenue Edouard Belin, 31400 Toulouse, France
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Abstract

The computation of the outermost layers of a star (the atmosphere) requires to solve in details the radiative transfer equation, whereas an analytical formula provides the radiative flux in optically thick layers, which is the case for the inner structure. Then, to have a complete stellar model from the center up to the optically thin layers, one should compute the inner structure on one hand and the uppermost part on the other, and connect the two in some way.

After a non-exhaustive review of what is done with other evolutionary codes, we will describe how we deal with the problems met while performing the junction of an inner structure computed with the Toulouse-Geneva Evolution Code (TGEC) and an ATLAS9 atmosphere. Global behaviour of some physical quantities when considering the complete model will be shown, along with the effect on the oscillation frequencies.

Type
Research Article
Information
European Astronomical Society Publications Series , Volume 63: New Advances in Stellar Physics: From Microscopic to Macroscopic Processes , 2013 , pp. 357 - 365
Copyright
© EAS, EDP Sciences, 2013

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References

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