The Oosterhoff dichotomy revisited. II - Pulsational constraints on the luminosity of RR Lyrae variables in OO II and OO I globular clusters

Details The Oosterhoff dichotomy revisited. II - Pulsational constraints on the luminosity of RR Lyrae variables in OO II and OO I globular clusters The Oosterhoff dichotomy revisited. II - Pulsational constraints on the luminosity of RR Lyrae variables in OO II and OO I globular clusters

Sep 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989a%26a...222..121c&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 222, no. 1-2, Sept. 1989, p. 121-124.

Physics

9

Dichotomies, Globular Clusters, Lyra Constellation, Stellar Evolution, Stellar Oscillations, Variable Stars, Histograms, Stellar Physics

Scientific paper

Period frequency histograms for RR Lyrae variables in the globular clusters M15, M3 and M5 are discussed in order to get information on the evolutionary characteristics of the pulsators, taken as representative of Oosterhoff group II and Oosterhoff group I, respectively. On the basis of theoretical relations linking pulsator period with stellar evolution parameters (luminosity, mass, effective temperature), a suitable scenario accounting for the different behavior of the pulsational properties among the three globular clusters is presented. The difference of period at the transition from fundamental to first harmonic mode occurring between M15 and M3 should mainly be due to a difference of the effective temperature where actually the transition occurs, whereas the similar variation observed between M3 and M5 should be attributed to a variation of the pulsator luminosity and/or mass.

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