The Oosterhoff dichotomy revisited. III - an empirical approach to the RRab/RRc transition line in M 15 and Omega Centauri

Details The Oosterhoff dichotomy revisited. III - an empirical approach to the RRab/RRc transition line in M 15 and Omega Centauri The Oosterhoff dichotomy revisited. III - an empirical approach to the RRab/RRc transition line in M 15 and Omega Centauri

Nov 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990a%26a...239..137c&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 239, no. 1-2, Nov. 1990, p. 137-141.

Statistics

Computation

Blue Stars, Computational Astrophysics, Giant Stars, Globular Clusters, Variable Stars, Stellar Luminosity, Stellar Magnitude, Stellar Mass, Stellar Temperature

Scientific paper

Available observations of ab- and c-type RR Lyrae variables in the galactic globular clusters M 15 and Omega Centauri are analyzed in order to obtain information on the transition line (TL) in the luminosity-effective temperature diagram separating fundamental and first harmonic pulsation. From the distribution of stars in the visual magnitude versus period diagram, it is possible to derive delta logT(TL)/delta log L equal to about + 0.24 in M 15 and delta logT(TL)/delta log L equal to about -0.08 in Omega Centauri. Despite this difference, it is suggested that, in both clusters, the ab/c transition occurs close to the red edge of the 'both instabilities' region as given by Stellingwerf (1975). Concerning Omega Centauri, it is further suggested that increasing the pulsator mass moves the transition line slightly toward the blue with a dependence of delta logT(TL)/delta log M equal to about 0.06.

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