Grids of massive stars with high mass loss rates. V. From 12 to 120 Mo at Z=0.001, 0.004, 0.008, 0.020 and 0.040 J/A+AS/103/97 J/A+AS/103/97 Grids of massive stars with high mass loss rates. V Grids of massive stars with high mass loss rates. V. From 12 to 120 Mo at Z=0.001, 0.004, 0.008, 0.020 and 0.040 G Meynet A Maeder G Schaller D Schaerer C Charbonnel Astron. Astrophys. Suppl. Ser. 103 97 1994 1994A&AS..103...97M Hertzsprung-Russell (HR diagram) stars: evolution stars: interiors stars: mass-loss Most outputs of massive star evolution critically depend on the mass loss rates. In order to broaden the comparison basis and to illustrate the effects of different mass loss rates, we have computed new sets of models, with initial masses between 12 and 120 M_{sun}_, and metallicities, Z, between 0.001 and 0.040, with a mass loss rate increased by a factor of two during the phases when the stellar winds are believed to be essentially driven by the radiation pressure. A moderate core-overshooting and the new radiative opacities from Iglesias et al. (1992) and Kurucz (1991) were taken into account. These models complete the homogeneous and extended theoretical database formed by the previous grids of this series, computed by Schaller et al. (1992) for Z=0.020 and Z=0.001, by Schaerer et al. (1992, 1993) for Z=0.008 and Z=0.040 and by Charbonnel et al. (1993) for Z=0.004. This paper closes this series. Of particular interest is the predicted behaviour of metal rich stars such as may be found in the inner regions of our Galaxy. New evolutionary connexions are found, in particular we show that the most massive and metal rich stars may spend a relatively long time as He and N enriched stars and may even end their evolution as white dwarfs.
120 M , z = 0.040, Mdot x 2 during the Main sequence and the wnl phases 85 M, z = 0.040, Mdot x 2 during the Main sequence and the wnl phases 60 M, z = 0.040, Mdot x 2 during the Main sequence and the wnl phases 40 M, z = 0.040, Mdot x 2 during the Main sequence and the wnl phases 25 M, z = 0.040, Mdot x 2 during the Main sequence and the wnl phases 20 M, z = 0.040, Mdot x 2 during the Main sequence and the wnl phases 15 M, z = 0.020, Mdot x 2 during the Main sequence and the wnl phases 12 M, z = 0.040, Mdot x 2 during the Main sequence and the wnl phases 120M, z = 0.040, Mdot x 2 during the Main sequence and the wnl phases 85 M, z = 0.001, Mdot x 2 during the Main sequence and the wnl phases 60 M, z = 0.020, Mdot x 2 during the Main sequence and the wnl phases 40 M, z = 0.020, Mdot x 2 during the Main sequence and the wnl phases 25 M, z = 0.020, Mdot x 2 during the Main sequence and the wnl phases 20 M, z = 0.020, Mdot x 2 during the Main sequence and the wnl phases 15 M, z = 0.020, Mdot x 2 during the Main sequence and the wnl phases 120 M, z = 0.008, Mdot x 2 during the Main sequence and the wnl phases 85 M, z = 0.008, Mdot x 2 during the Main sequence and the wnl phases 60 M, z = 0.008, Mdot x 2 during the Main sequence and the wnl phases 40 M, z = 0.008, Mdot x 2 during the Main sequence and the wnl phases 25 M, z = 0.008, Mdot x 2 during the Main sequence and the wnl phases 20 M, z = 0.008, Mdot x 2 during the Main sequence and the wnl phases 15 M, z = 0.008, Mdot x 2 during the Main sequence and the wnl phases 120 M, z = 0.004, Mdot x 2 during the Main sequence and the wnl phases 85 M, z = 0.004, Mdot x 2 during the Main sequence and the wnl phases 60 M, z = 0.004, Mdot x 2 during the Main sequence and the wnl phases 40 M, z = 0.004, Mdot x 2 during the Main sequence and the wnl phases 25 M, z = 0.004, Mdot x 2 during the Main sequence and the wnl phases 20 M, z = 0.004, Mdot x 2 during the Main sequence and the wnl phases 120 M, z = 0.001, Mdot x 2 during the Main sequence and the wnl phases 85 M, z = 0.001, Mdot x 2 during the Main sequence and the wnl phases 60 M, z = 0.001, Mdot x 2 during the Main sequence and the wnl phases 40 M, z = 0.001, Mdot x 2 during the Main sequence and the wnl phases 25 M, z = 0.001, Mdot x 2 during the Main sequence and the wnl phases NB number of selected point --- Age age yr Mass actual mass in solar masses Sun logL log(luminosity) in solar units Sun logTe log(effective temperature) K X H surface abundance (mass fraction) --- Y He surface abundance (mass fraction) --- C12 12C surface abundance (mass fraction) --- C13 13C surface abundance (mass fraction) --- N14 14N surface abundance (mass fraction) --- O16 16O surface abundance (mass fraction) --- O17 17O surface abundance (mass fraction) --- O18 18O surface abundance (mass fraction) --- Ne20 20Ne surface abundance (mass fraction) --- Ne22 22Ne surface abundance (mass fraction) --- QCC core mass fraction --- logTu log(uncorrected Teff) (WR stars only) K logMdot log(mass loss rate) Sun/yr log(rho_c) log(central density) g/cm3 logTc log(central temperature) K Xc H central abundance (mass fraction) --- Yc He central abundance (mass fraction) --- C12c 12C central abundance (mass fraction) --- C13c 13C central abundance (mass fraction) --- N14c 14N central abundance (mass fraction) --- O16c 16O central abundance (mass fraction) --- O17c 17O central abundance (mass fraction) --- O18c 18O central abundance (mass fraction) --- Ne20c 20Ne central abundance (mass fraction) --- Ne22c 22Ne central abundance (mass fraction) --- Patricia Bauer CDS 1993Sep29 J_A+AS_103_97.xml