EVOLUTIONARY SEQUENCES OF STELLAR MODELS WITH NEW RADIATIVE OPACITIES.2. Z = 0.02

We present a large grid of stellar models computed with the most recen t radiative opacities by Iglesias et al. (1992). The chemical composit ion, typical of the solar vicinity, is X = 0.700, Y = 0.28, and Z = 0. 020. The evolutionary tracks have initial masses in the range 0.6 M. t o 120 M. and extend from the zero age main sequence (ZAMS) to the begi nning of the thermally pulsing regime of the asymptotic giant branch p hase (TPAGB) for low and intermediate mass stars, and to the central C -ignition for higher masses. The computations are performed adopting a moderate non local overshoot from convective regions. Low and interme diate mass stars calculated at constant mass because mass loss during the red giant (RGB) and asymptotic giant branch (AGB) phases can be ea sily included following the standard analytical procedure, while massi ve stars (M greater-than-or-equal-to 12 M.) are evolved in presence of mass loss by stellar winds. The remaining physical input of the stell ar models, i.e. nuclear reaction rates, nucleosynthesis network, neutr ino energy losses, boundary conditions in the outer layers etc., is as in Alongi et al. (1992), but for the mixing length parameter in the o utermost super-adiabatic convection. With the new opacities, the lumin osity and effective temperature of the Sun are matched by our model st ar with the age of 4.7 10(9) yr by adopting a mixing length parameter alpha = 1.63 instead of 1.5 as found by Alongi et al. (1992) with the Los Alamos opacity by Huebner et al. (1977). For purposes of compariso n, two additional samples of models are presented with different detai l. The first sample contains models calculated with the same physical input (chemical composition, opacity, etc) as above but the classical mixing scheme (no overshoot and semiconvection during the core He-burn ing phase). The models of the second group, whose properties are preen ted here limited to the lifetimes of the major evolutionary phases, ar e calculated with the same chemical composition, convective overshoot, and the opacity by Huebner et al. (1977). The results of all the mode ls are given in extensive tables. In addition to this, we shortly disc uss some general properties of the models such as the evolutionary pat h in the Hertzsprung-Russell diagram (HRD), the lifetimes of the vario us phases, and the variation of the surface abundance induced by exter nal convection and mass loss by stellar wind.