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Modelling Time-Dependent Diffusion in Am Star Envelopes

Published online by Cambridge University Press:  12 April 2016

G. Alecian
G. Alecian*
Affiliation:
DAEC, URA173-CNRS, Observatoire de Paris, Section de Meudon, F-92195 MEUDON CEDEX, FRANCE

Abstract

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We study the diffusion process occurring just below the superficial convection zone of Am stars, improving the methods used sofar. We are now able to compute, in a more realistic way, the evolution of the concentrations during the stay of the stars on the main sequence for a large number of elements. This allows to better constrain the different properties (mass loss, depth of the superficial convection zone, transition between convection and radiative zone) entering the modelling of Am stars in the framework of a diffusion-dominant description.

Type
III. Input physics for stellar structure
Information
International Astronomical Union Colloquium , Volume 137: Inside the Stars , 1993 , pp. 272 - 274
Copyright
Copyright © Astronomical Society of the Pacific 1993

References

Alecian, G.: 1986, Astron. Astrophys., 168, 204 Google Scholar
Alecian, G., Artru, M.C.: 1990, Astron. Astrophys., 234, 323 Google Scholar
Alecian, G.: 1990, IAU Symposium N° 145 on “Evolution of Stars: the photospheric abundance connection”Google Scholar
Burkhart, C., Coupry, M.F.: 1991, Astron. Astrophys., 249, 205 Google Scholar
Kurucz, R.L., Peytremann, E.: 1975, A table of semi Empirical gf Values, Smithonian Astrophys. Obs. Spec. Rept. N° 362Google Scholar