Evolutionary sequences of stellar models with new radiative opacities. IV. Z = 0.004 and Z=0.008 J/A+AS/105/29 J/A+AS/105/29 Evolutionary sequences IV. Evolutionary sequences of stellar models with new radiative opacities. IV. Z = 0.004 and Z=0.008 F Fagotto A Bressan G Bertelli C Chiosi Astron. Astrophys. Suppl. Ser. 105 29 1994 1994A&AS..105...29F stars: evolution stars: interiors We present detailed tabulations of two large grids of stellar models with the initial chemical compositions [Y=0.240, Z=0.004] and [Y=0.250, Z=0.008], computed with the most recent radiative opacities (OPAL) by Iglesias et al. (1992). This paper continues the series initiated by Bressan et al. (1993) for the grid with [Y=0.280, Z=0.020], the reference solar like abundances, followed by Fagotto et al. (1994a) for the grids with compositions [Y=0.230, Z=0.0004] and [Y=0.352, Z=0.05]. The tracks span a wide range of initial masses from 0.6M_{sun}_ to 120M_{sun}_ and extend from the zero age main sequence (ZAMS) till very advanced evolutionary phases. Specifically, low- and intermediate-mass stars are followed till the beginning of the thermally pulsing regime of the asymptotic giant branch phase (TP-AGB), while massive stars are followed till the core C-ignition. The models of low- and intermediate-mass stars are calculated at constant mass, whereas those of massive stars are followed in presence of mass loss by stellar wind incorporating a suitable dependence on the metallicity. The results for all the models are given in extensive tables which summarize also the lifetimes of the various phases and the variations of the surface abundances by dredge-up phenomena and mass loss by stellar wind. The salient features brought by the different metallicity and helium content are briefly outlined. In virtue of their large coverage of masses, evolutionary phases, and chemical compositions, such grids of evolutionary tracks are basic to studies of population synthesis. In particular they are suited to interpret the CMDs of metal-rich globular clusters and of the typical stellar content of the Large Magellanic Cloud.
Evolutionary sequences of low mass stars up to the tip of the RGB. 0.6 < M < 1.8 for z=0.004 Evolutionary sequences of low mass stars up to the tip of the RGB. 0.6 < M < 1.8 for z=0.008 Evolutionary sequences of low mass stars during the core-helium burning and EAGB phases. 0.5 < M < 1.8 for z=0.004 Evolutionary sequences of low mass stars during the core-helium burning and the EAGB phases. 0.5 < M < 1.8 for z=0.008 Evolutionary sequences of intermediate stars up to the TPAGB or carbon-ignition. 1.9 < M < 9.0 for z=0.004 Evolutionary sequences of intermediate stars up to the TPAGB or carbon-ignition. 2.0 < M < 9.0 for z=0.008 m Initial mass Sun Age Age of models yr log(L) Total luminosity Sun log(Teff) Effective temperature K log(G) Surface gravity cm/s2 log(Tc) Central temperature K log(rho_c) Central density g/cm3 COMP Central abundance (by mass) of hydrogen or helium --- X_C Central abundance of 12C --- X_O Central abundance of 16O --- Conv Fractionary mass of the convective core (inclusive of overshoot) --- Q_disc Fractionary mass of the first mesh point where the chemical composition differs from the surface value --- log(L_H) Hydrogen luminosity Sun Q1_H Fractionary mass of the inner border of the hydrogen rich region --- Q2_H Fractionary mass of the outer border of the H-burning region. The boundary is taken where the nuclear energy generation rate becomes greater than a suitable value --- log(L_He) Helium luminosity Sun Q1_He Fractionary mass of the inner border of the He-burning region (when greater than zero He-burning is in a shell). The boundary is taken where the nuclear energy generation rate becomes greater than a suitable value --- Q2_He Fractionary mass of the upper border of the He-burning region. The boundary is taken as above. --- log(L_C) Carbon luminosity Sun log(L_nu) Neutrinos luminosity (absolute value) Sun Q_Tmax Fractionary mass of the point where the temperature attains the maximum value --- Evolutionary sequences for massive stars. 12 < M < 120 for z=0.004 Evolutionary sequences for massive stars. 12 < M < 120 for z=0.008 m Initial mass Sun Age Age of models yr M Current value of the mass Sun log(L) Total luminosity Sun log(Teff) Effective temperature K log(G) Surface gravity cm/s2 log(Tc) Central temperature K log(rho_c) Central density g/cm3 COMP Central abundance of hydrogen or helium by mass --- X_C Central abundance of 12C --- X_O Central abundance of 16O --- Conv Fractionary mass of the convective core (inclusive of overshoot) --- Q_disc Fractionary mass of the first mesh point where the chemical composition differs from the surface value --- log(L_H) Hydrogen luminosity Sun Q1_H Fractionary mass of the inner border of the hydrogen rich region --- log(L_He) Helium luminosity Sun log(M_dot) Absolute value of the mass loss rate Sun/yr X_sur Surface abundance by mass of 1H --- Y_sur Surface abundance by mass of 4He --- XC_sur Surface abundance by mass of 12C --- XN_sur Surface abundance by mass of 14N --- XO_sur Surface abundance by mass of 16O --- table1.texLatex version of table1(a,b) table2.texLatex version of table2(a,b) table3.texLatex version of table3(a,b) table4.texLatex version of table4(a,b) Patricia Bauer CDS 1994Jan21 J_A+AS_105_29.xml