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Carbon Abundances in Planetary Nebulae in the Galactic Bulge

Published online by Cambridge University Press:  25 April 2016

B. Louise Webster
B. Louise Webster*
Affiliation:
School of Physics, University of New South Wales
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Extract

The galactic nuclear bulge is a well defined population, but it is one that is relatively difficult to study in detail because its members never stray into the solar vicinity and they are both distant and obscured. Mould (1982) has summarized much of our knowledge of the masses and composition of stars in the bulge. The red giants resemble those in metal-rich old open clusters and the late M giants are either younger than galactic globular clusters or super-metal-rich or both. Whitford and Rich (1983) have demonstrated the existence of K-giants that are super-metal-rich in iron and Wood and Bessell (1983) have interpreted the properties of a sample of long period variables in the bulge as those of a young, super-metal-rich population.

Type
Contributions
Information
Publications of the Astronomical Society of Australia , Volume 5 , Issue 4 , 1984 , pp. 535 - 537
Copyright
Copyright © Astronomical Society of Australia 1984

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