Abstract
The general characteristics of Mira variables are reviewed with particular emphasis on the PL and other relations which they obey. It is highly likely that these stars represent the termination of the AGB. On this assumption a comparison of pulsation masses with evolutionary theory allows a rough estimate to be made of the mass ejected as a planetary nebula. The luminosities of Miras in the LMC, globular clusters and the galactic bulge are closely the same at a given period. Most IRAS sources in the galactic bulge are probably Miras with low temperature shells. The bulge Miras are distinct from the non-variable (or low amplitude) late-type M giants found in the bulge by Blanco et al. There is at present no compelling reason to assume that the latter are AGB stars. Few (IRAS) Miras in the bulge have luminosities greater than MBol = -4.7 corresponding to a period of ~400 days and an age of 5–8 Gyr. There is at present no evidence that any substantial part of the general bulge population has an age less than ~5 Gyr.
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Feast, M.W., Whitelock, P.A. (1987). Mira Variables and the Galactic Bulge Population. In: Kwok, S., Pottasch, S.R. (eds) Late Stages of Stellar Evolution. Astrophysics and Space Science Library, vol 132. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-3813-7_3
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DOI: https://doi.org/10.1007/978-94-009-3813-7_3
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