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Chemical Evolution of the Magellanic Clouds

Published online by Cambridge University Press:  19 July 2016

B. Barbuy ,
J. A. de Freitas Pacheco  and
T. Idiart
B. Barbuy
Affiliation:
Universidade de São Paulo C.P. 3386, Sao Paulo 01060-970, Brazil
J. A. de Freitas Pacheco
Affiliation:
Observatoire de la Côte d'azur BP 4229, 06304 Nice Cedex 4, Prance
T. Idiart
Affiliation:
Observatoire de la Cote d'Azur BP 4229, 06304 Nice Cedex 4, Prance

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Chemical evolution studies of the Clouds based on detailed abundance analyses are essentially limited nowadays to young objects like HII regions (Dufour 1984; Garnett et al. 1995), planetary nebulae (e.g. de Freitas Pacheco et al. 1993), supernova remnants (Russell & Dopita 1990) and supergiant stars either of F-K type (Hill et al. 1995) or B ones (e.g. Rolleston et al. 1996 and references therein). One exception to this was presented by Dopita et al. (1997) where HST data permitted to date planetary nebulae nuclei and to present an age vs. metallicity model.

Type
Conference Papers in order of Presentation
Information
Symposium - International Astronomical Union , Volume 187: Cosmic Chemical Evolution , 2002 , pp. 195 - 199
Copyright
Copyright © 2002 

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