IV. From 0.8 to 125: high metallicities (Z = 0.04–0.10)
Instituto de Astrofísica de Andalucía, CSIC, Apartado 3004, 18080 Granada, Spain e-mail: firstname.lastname@example.org
Accepted: 28 January 2007
Aims.The aim of the present grid of stellar models is to complete our previous calculations and provide a tool for investigating the astrophysical properties of eclipsing binaries, stellar clusters, galactic bulges, and elliptical galaxies with a high metal content.
Methods.To explore the applicability of high metallic models, we have computed three grids: (X, , (0.58, 0.06), and (0.46, 0.10). For all these grids, we adopted an enrichment law , as in our previous papers on this subject. The input physics is almost the same as adopted in our earlier work except for some numerical details, recent measurement of the rate for the reaction 14N()15O, and the recent mass-loss rate for the Wolf-Rayet stages.
Results.Two high-metallicity clusters, NGC 6253 and NGC 6791, were used to test the present calculations with very satisfactory results. On the other hand, as this series of grids was mainly designed to investigate the tidal evolution of close binaries, we analyse the present status of circularization times in both clusters and isolated binaries. The present models (90 tables) can be retrieved from the CDS via anonymous ftp.
Key words: binaries: eclipsing / stars: evolution / stars: abundances / stars: rotation
© ESO, 2007