MASS-LOSS DURING THE RR LYRAE PHASE OF THE HORIZONTAL-BRANCH - MASS DISPERSION ON THE HORIZONTAL-BRANCH AND RR LYRAE PERIOD CHANGES

Mass loss on the horizontal branch has been invoked in the literature to explain such phenomena as the color (mass) dispersion of the horizo ntal branch and the observed distribution of period changes in RR Lyra e stars. To test these claims, the Yale stellar evolution code was use d to evolve horizontal branch models of masses 0.64, 0.66, 0.68, 0.70, and 0.72 M. with Z of 0.001, core mass of 0.4893, main-sequence heliu m abundance of 0.23, and constant mass loss rates of 0, 10(-10), 5 x 1 0(-10), and 10(-9) M. yr-1. Mass loss was assumed to occur only in the instability strip, where a mechanism is most likely to exist. Synthet ic horizontal branches, constructed from the models, show that mass lo ss on the horizontal branch cannot produce the observed color dispersi on even for the highest mass-loss rate of 10(-9) M, yr-1. Mass loss is unlikely to occur at a higher rate without significant effects on the horizontal branch morphology, which would destroy the good agreement between standard synthetic models without mass loss and observed horiz ontal branches. Periods and period changes were calculated for all mod els. The period changes are not significantly larger for models with m ass loss. The effect of mass loss in clusters of other metallicities i s discussed.