Abstract
Planetary Nebulae have proven to be an essential key to understand the long term chemical enrichment of the interstellar medium due to low mass stars. They allow to study the original abundances of the star, and the effect of the star on the interstellar medium. Blue compact dwarf galaxies are known to host violent star formation in very heavy element depleted environments. They also show traces of past star formation (Doublier et al., 1999; 2001), including AGB starsand red giants which are responsible for long term enrichment. However, models fails to reproduce the low metallicities observed if those stars are taken into account. We observed PNe in BCDGs, and made a comparative study of the abundances in the HII regions and of the PNe.
This is a preview of subscription content, log in via an institution to check access.
Similar content being viewed by others
References
Doublier, V., Caulet, A. and Comte, G.: 1999, Multi-spectral study of a new sample of Blue Compact Dwarf Galaxies. II. B and R surface photometry of 22 southern objects, A&AS 138, 213–245.
Doublier, V., Caulet, A. and Comte, G.: 2001, The 1 to 2.5 µ broad band emission of blue compact dwarf galaxies, A&A 367, 33–45.
Maeder, A. and Meynet, G.: 2000, The evolution of rotating stars, ARA&A 38, 143–190.
Thuan, T.X., Izotov, Y.I. and Lipovetsky, V.A.: 1995, Heavy element abundances in a new sample of low-metallicity blue compact galaxies, ApJ 445, 108–123.
Author information
Authors and Affiliations
Rights and permissions
About this article
Cite this article
Doublier, V. PNE: The Key to Chemical Evolution in BCDGs. Astrophysics and Space Science 281, 211–212 (2002). https://doi.org/10.1023/A:1019525814475
Issue Date:
DOI: https://doi.org/10.1023/A:1019525814475