Grids of stellar models V.

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. (1992ApJ...397..717I) 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, Cat. J/A+AS/96/269) for Z=0.020 and Z=0.001, by Schaerer et al. (1992, Cat.