On the Two Oosterhoff Groups of Globular Clusters

The observational evidence leading to the classification, following Oosterhoff, of globular clusters containing RR Lyrae stars into two distinct groups, is summarized and discussed in the light of results of stellar-evolution theory and pulsation theory. The dichotomy is caused, at least in part, by a dichotomy in the "transition period" between the type ab and type c stars which reflects a difference in effective temperature at the transition point. When this difference is accounted for, there remains a smaller average difference between the groups, although no longer a clear dichotomy, that is probably a mass and luminosity effect. If this remaining difference is interpreted as a luminosity effect the average difference in luminosity between the two Oosterhoff groups is at most 0.1 mag. It is suggested that Christy's theoretical relationship between transition period and luminosity cannot be valid, at least not for clusters of different Oosterhoff groups. It is conjectured that the transition-temperature dichotomy may be a reflection of different predominant directions of evolution through the instability strip, accompanied by a hysteresis effect in the pulsation. Subject headings: globular clusters - pulsation - RR Lyrae stars