J/A+AS/105/39 J/A+AS/105/39 Evolutionary sequences V. F Fagotto A Bressan G Bertelli C Chiosi Astron. Astrophys. Suppl. Ser. 105 39 1994 1994A&AS..105...39F J/A+AS/100/647 : (II: Z = 0.02) J/A+AS/104/365 : (III: Z = 0.0004 and Z = 0.05) J/A+AS/105/29 : (IV: Z = 0.004 and Z = 0.008) J/A+AS/105/39 : (V: Z = 0.10) Abundances Models, evolutionary stars: evolution stars: interiors We present detailed tabulations of a large grid of stellar models with initial chemical compositions [Y=0.475, Z=0.1] computed with the radiative opacities by Huebner et al. (1977) and convective overshoot. This choice of the opacity is due to the high metallicity in use, because the Livermore Library of radiative opacities (Iglesias et al. 1992) did not contain tabulations for Z=0.1. The tracks span the range of initial masses from 0.6M_{sun}_ to 9M_{sun}_ and extend from the zero age main sequence (ZAMS) till very advanced evolutionary phases. Specifically, low- and intermediate-mass stars are followed either till the white dwarf (WD) or late stages of the early asymptotic giant branch (AGB) phase, depending on the mass of the star and on details of the evolutionary behaviour discussed in the text. Massive stars are calculated till core C-ignition. The critical masses separating low- from intermediate-, and intermediate-mass from massive stars are M_HeF_=1.3M_{sun}_ andM_up_=4M_{sun}_, respectively. All the models are calculated at constant mass. 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 limited to the first dredge-up. The stellar models presented here are particularly suited to interpret the CMDs of very metal-rich clusters and the stellar content of elliptical galaxies. However we warn the reader that, because of the opacity, these models are not fully homogeneous with the others of the same series by Bressan et al. (1993) and Fagotto et al. (1994a,b) that are calculated with the Livermore opacity.

m Initial mass solMass Age Age of models yr log(L) Total luminosity [solLum] 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 [solLum] 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 [solLum] 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 [solLum] log(L_nu) Neutrinos luminosity (absolute value) [solLum] Q_Tmax Fractionary mass of the point where the temperature attains the maximum value --- table1.texLaTex version of table1 table2.texLaTex version of table2 table3.texLaTex version of table3 Patricia Bauer CDS 1994Jan20 UNKNOWN UNKNOWN * 22-Oct-1997: table2 completed with missing models of masses from 0.7 to 1.3 J_A+AS_105_39.xml