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Long-period variables and carbon stars in the Galactic Bulge

Published online by Cambridge University Press:  07 August 2017

Patricia Whitelock
Patricia Whitelock*
Affiliation:
South African Astronomical Observatory, P O Box 9, Observatory, Cape 7935, South Africa October 12, 1992

Abstract

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The review covers the properties of red variables in globular clusters and the Galactic Bulge. Details are given of our current understanding of the Mira evolutionary phase. There is evidence that Miras in the LMC and the Bulge occupy different parts of the instability strip but obey the same PLC relation. The Bulge contains at least 2 × 104 Miras of which 100 or so have luminosities in excess of Mbol = — 5 mag. The Mira phase lasts more than 105 yr. These objects originate from stars with a wide range of metallicity, but it is currently unclear if the most metal-rich stars reach the top of the AGB to become Miras. Preliminary data suggest that the distribution of the Miras along the minor axis of the Bulge is different from that of the late-M stars but similar to the 2.4 μm luminosity.

Our knowledge of the Bulge carbon stars is briefly reviewed. It is suggested that, by analogy with the carbon-rich dwarfs, these stars are probably best understood as the products of binary evolution.

Keywords

Galactic BulgeMira VariablesLPVsIRAS sourcesCarbon StarsMetallicity Gradients
Type
Invited Reviews
Information
Symposium - International Astronomical Union , Volume 153: Galactic Bulges , 1993 , pp. 39 - 56
Copyright
Copyright © Kluwer 1993 

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