THE RRd MASSES REVISITED
نویسندگان
چکیده
We reexamine the RRd mass determination using both new and previously existing linear pulsation models. Our conclusion is that the weight of evidence remains strongly with the" canonical" values (0.55 M (:) for Oosterhoff I clusters and 0.65 M 0 for Oosterhoff II clusters), unless the Population II metal opacities turn out to be very high. Subject headings: stars: interiors stars: pulsation stars: RR Lyrae
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