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Published online by Cambridge University Press: 12 April 2016
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.