Don A. VandenBerg (1), Peter A. Bergbusch (2), Aaron Dotter (3), Jason W. Ferguson (4), Georges Michaud (5), Jacques Richer (6) & Charles R. Proffitt (7) ((1) Department of Physics & Astronomy, University of Victoria, P.O. Box 3055, Victoria, B.C., V8W 3P6, Canada; (2) Department of Physics, University of Regina, Regina, Saskatchewan, S4S 0A2, Canada; (3) Department of Physics & Astronomy, University of Victoria, P.O. Box 3055, Victoria, B.C., V8W 3P6, Canada; (4) Department of Physics, Wichita State University, Wichita KS 67260-0032, U.S.A; (5) Département de Physique, Université de Montréal, Montréal, Quebec, H3C 3J7, Canada; (6) Département de Physique, Université de Montréal, Montréal, Quebec, H3C 3J7, Canada; (7) Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, U.S.A. )
Recent work has shown that most globular clusters have at least two chemically distinct components, as well as cluster-to-cluster differences in the mean [O/Fe], [Mg/Fe], and [Si/Fe] ratios at similar [Fe/H] values. In order to investigate the implications of variations in the abundances of these and other metals for H-R diagrams and predicted ages, grids of evolutionary sequences have been computed for scaled solar and enhanced alpha-element mixtures, and for mixtures in which the assumed [m/Fe] value for each of the metals C, N, O, Ne, Na, Mg, Si, S, Ca, and Ti has been increased, in turn, by 0.4 dex at constant [Fe/H]. These tracks, together with isochrones for ages from 6 to 14 Gyr, have been computed for -3.0 < [Fe/H] < -0.6, with helium abundances Y = 0.25, 0.29, and 0.33 at each [Fe/H] value, using upgraded versions of the Victoria stellar structure program and the Regina interpolation code, respectively. Turnoff luminosity versus age relations from isochrones are found to depend almost entirely on the importance of the CNO-cycle, and thereby mainly on the abundance of oxygen. Since C, N, and O, as well as Ne and S, do not contribute significantly to the opacities at low temperatures and densities, variations in their abundances do not impact the Teff scale of red giants. The latter is a strong function of the abundances of only Mg and Si (and Fe, possibly to a lesser extent), because they are so abundant and because they are strong sources of opacity at low temperatures. For these reasons, Mg and Si also have important effects on the temperatures of main-sequence stars. Due to their low abundances, Na, Ca, and Ti are of little consequence for stellar models. The effects of varying the adopted solar metals mix and the helium abundance at a fixed [Fe/H] are also briefly discussed.
Complete preprint ==> http://arxiv.org/abs/1206.1820