RR Lyrae stars in Galactic globular clusters. II. A theoretical approach to variables in M3

Details RR Lyrae stars in Galactic globular clusters. II. A theoretical approach to variables in M3 RR Lyrae stars in Galactic globular clusters. II. A theoretical approach to variables in M3

2003-06-18

arxiv.org/abs/astro-ph/0306356v1

Astrophys.J.596:299-313,2003

Astronomy and Astrophysics

Astrophysics

29 pages, 20 postscript figures, accepted for publication on ApJ

Scientific paper

10.1086/377641

We present predicted relations connecting pulsational and evolutionary parameters, as based on a wide set of convective pulsating models of RR Lyrae stars with Z=0.001, Y=0.24 and mass and luminosity suitable for the ``old'' (age $>$ 8 Gyr) variables observed in globular clusters. The relations are collated with sound constraints on the mass of pulsators, as inferred from up-to-date evolutionary models of horizontal branch stars, in order to provide a self-consistent theoretical framework for the analysis of observed variables. The theoretical predictions are tested through a detailed comparison with measurements of RR Lyrae stars in the globular cluster M3. We show that the predicted relations satisfy a variety of observed data, thus providing a "pulsational" route to the determination of accurate distances to RR Lyrae-rich globular clusters with intermediate metal content. We discuss the effect of different physical inputs in evolutionary computations, as well as of different bolometric corrections adopted to convert bolometric luminosity into absolute magnitude. We show that the constraints inferred by pulsation theory support the large value of the mixing-length parameter adopted to fit observed RGB, but, at the same time, they would yield that the luminosity of updated HB models is too bright. Such discrepancy is significantly reduced if element diffusion is properly taken into account.

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