Evolution and period change in RR Lyr variables of the globular cluster M 3
arXiv:1806.06836 · doi:10.1134/S1063773718100018
Abstract
The grid of evolutionary tracks of population II stars with initial masses from to and chemical composition of the globular cluster M 3 is computed. Selected models of horizontal branch stars were used as initial conditions for solution of the equations of radiation hydrodynamics and time--dependent convection describing radial stellar oscillations. The boundaries of the instability strip on the Herztsprung--Russel diagram were determined using nearly 100 hydrodynamic models of RR Lyr pulsating variables. For each evolutionary track crossing the instability strip the pulsation period was determined as a function of evolutionary time. The rate of period change of most variables is shown to range within . Theoretical estimate of the mean period change rate obtained by the population synthesis method is and agrees well with observations of RR Lyr variables of the globular cluster M 3.
11 pages, 3 figures, accepted to Astronomy Letters
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