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Comparison of the abundances in the stars and in the HII regions of the Magellanic Clouds

Published online by Cambridge University Press:  19 July 2016

M. Spite  and
F. Spite
M. Spite
Affiliation:
Observatoire de Paris-Meudon, 92195 Meudon Cedex, France
F. Spite
Affiliation:
Observatoire de Paris-Meudon, 92195 Meudon Cedex, France

Abstract

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Both HII regions and F supergiants are young objects, and are, therefore, supposed to have the same abundances for all elements, especially for C, O and S, which offer a good opportunity to check the abundance determinations made by two different techniques. For oxygen and sulfur the agreement is good but the discrepancy of the carbon abundance cannot be easily explained.

Type
Stellar Evolution
Information
Symposium - International Astronomical Union , Volume 148: The Magellanic Clouds , 1991 , pp. 372 - 373
Copyright
Copyright © Kluwer 1991 

References

Dufour, R.J. (1984), IAU Symp. 108 Structure and Evolution of the Magelllanic Clouds , van den Bergh, S. and de Boer, K.S. (eds.) (Reidel: Dordrecht) p. 353.Google Scholar
Kurucz, R.L. (1979), Astrophys. J. Suppl. Ser. 40, 1.Google Scholar
Russell, S.C., Bessell, M.S. (1989), Astrophys. J. Suppl. Ser. 70, 865.Google Scholar
Spite, F., Spite, M., François, P. (1989a), Astron. Astrophys. 210, 25.Google Scholar
Spite, M., Barbuy, B., Spite, F. (1989b), Astron. Astrophys. 222, 35.Google Scholar
Spite, M., Spite, F. (1990), Astron. Astrophys. in press.Google Scholar