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The Metal-Rich RR Lyraes: Their Origin and Bearing on the Age and Helium Abundance of the Galactic Disk

Published online by Cambridge University Press:  12 April 2016

Robert P. Kraft
Robert P. Kraft*
Affiliation:
Lick Observatory, Board of Studies in Astronomy and Astrophysics, University of California, Santa Cruz 95064

Abstract

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We consider further the question of the origin and evolution of metal-rich RR Lyraes (MR-RR’s) in the solar vicinity, continuing the discussion begun by Taam, et al (1976) who showed that MR-RR’s descend from red giants of Eggen’s old disk population. If an old disk giant (ODG) is similar to a giant in a galactic cluster like NGC 188, then it must lose~0.5 M⊙ if it is to pump the HR-RR domain; thus the probability that an ODG will metamorphose into an RR Lyrae is about 1/200th the probability that its metal-poor (halo) counterpart will do so, else the sky would be full of bright MR-RR’s.

Type
Part III: Evolved Stars
Information
International Astronomical Union Colloquium , Volume 42: The Interaction of Variable Stars with their Environment , 1977 , pp. 521 - 558
Copyright
Copyright © Veröff. Der Remeis-Sterwarte 1977

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