Evolutionary Sequences of Stellar Models with New Radiative Opacities. II. Z = 0.02 J/A+AS/100/647 J/A+AS/100/647 Evolutionary Sequences of Stellar Models with New Evolutionary Sequences of Stellar Models with New Radiative Opacities. II. Z = 0.02 A Bressan F Fagotto G Bertelli C Chiosi Astron. Astrophys. Suppl. Ser. 100 647 1993 1993A&AS..100..647B Hertzsprung-Russell (HR diagram) stars: abundances stars: evolution stars: imaging stars: interiors A large grid of stellar models computed with the most recent radiative opacities by Iglesias et al. (1992) is presented. The evolutionary tracks have initial masses in the range 0.6 to 120 solar masses and extend from the ZAMS to the beginning of the thermally pulsing regime of the AGB for low and intermediate mass stars, and to the central C-ignition for higher masses. Two smaller samples of stellar models are also presented. The first deals with models of the same chemical composition and opacity but calculated with the classical scheme of mixing. They are meant to provide the necessary tool for discriminating among the two types of mixing. The other sample contains models of the same composition calculated with overshoot and classical radiative opacities by Huebner et al. (1977).
Table 1, M=0.60 Table 1, M=0.70 Table 1, M=0.80 Table 1, M=0.90 Table 1, M=1.00 Table 1, M=1.1 Table 1, M=1.2 Table 1, M=1.3 Table 1, M=1.4 Table 1, M=1.5 Table 1, M=1.6 Table 1, M=1.7 Table 1, M=1.8 Table 1, M=1.9 Table 1, M=2.0 Table 2, M=0.50 Table 2, M=0.55 Table 2, M=0.60 Table 2, M=0.70 Table 2, M=0.80 Table 2, M=0.90 Table 2, M=1.0 Table 2, M=1.1 Table 2, M=1.2 Table 2, M=1.3 Table 2, M=1.4 Table 2, M=1.5 Table 2, M=1.6 Table 2, M=1.7 Table 2, M=2.0 Table 3, M=2.2 Table 3, M=2.5 Table 3, M=3.0 Table 3, M=4.0 Table 3, M=5.0 Table 3, M=6.0 Table 3, M=7.0 Table 3, M=9.0 Table 5, M=2.5 Table 5, M=3.0 Table 5, M=4.0 Table 5, M=5.0 Table 5, M=7.0 Table 5, M=9.0 Age Age of models yr log.L log of total luminosity Sun log.Te log of effective temperature K log.g log of surface gravity cm/s2 log.Tc log of central temperature K log.rho_c log of central density g/cm3 Comp central abundance (by mass) of H or He --- XC central abundance of 12 C --- XO central abundance of 16 O --- 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 log of H luminosity Sun Q1_H fractionary mass of the inner border of the H-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 log of He 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 log of C luminosity Sun log.L_nu log of neutrinos luminosity (absolute value) Sun Q_Tmax fractionary mass of the point where the temperature attains the maximum value --- Table 4, M=12 Table 4, M=15 Table 4, M=20 Table 4, M=30 Table 4, M=40 Table 4, M=60 Table 4, M=100 Table 4, M=120 Table 5, M=12 Table 5, M=15 Table 5, M=20 Age Age of models yr M current value of the Mass Sun log.L log of total luminosity Sun log.Te log of effective temperature K log.g log of surface gravity cm/s2 log.Tc log of central temperature K log.rho_c log of central density g/cm3 Comp central abundance (by mass) of H or He --- XC central abundance of 12 C --- XO central abundance of 16 O --- 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 log of H luminosity Sun Q1_H fractionary mass of the inner border of the H-rich region --- log.L_He log of He luminosity Sun log.Mdot log of absolute value of mass loss rate Sun/yr X_sur surface abundance (by mass) of 1 H --- Y_sur surface abundance (by mass) of 4 He --- XC_sur surface abundance (by mass) of 12 C --- XN_sur surface abundance (by mass) of 14 N --- XO_sur surface abundance (by mass) of 16 O --- table1.texTable 1, LaTeX table2.texTable 2, LaTeX table3.texTable 3, LaTeX table4.texTable 4, LaTeX table5.texTable 5, LaTeX CDS 1993Feb09 J_A+AS_100_647.xml