J/A+AS/106/275 J/A+AS/106/275 Theoretical isochrones G Bertelli A Bressan C Chiosi F Fagotto E Nasi Astron. Astrophys. Suppl. Ser. 106 275 1994 1994A&AS..106..275B Hertzsprung-Russell (HR diagram) stars: evolution stars: fundamental parameters stars: interiors We present large grids of theoretical isochrones for the initial chemical compositions [Z=0.0004, Y=0.23], [Z=0.004, Y=0.24], [Z=0.008, Y=0.25], [Z=0.02, Y=0.28], and [Z= 0.05, Y=0.352] and ages in the range 4 10^6^ yr to 16 10^9^ yr. These isochrones are derived from stellar models computed with the most recent radiative opacities by Iglesias et al. (1992). In addition to this we present another set with chemical composition [Z=0.001, Y=0.23] based on models calculated with the radiative opacities by Huebner et al. (1977). All the stellar models are followed from the zero age main sequence (ZAMS) to the central carbon ignition for massive stars or to the beginning of the thermally pulsing regime of the asymptotic giant branch phase (TP-AGB) for low and intermediate mass stars. For each isochrone, we give the current mass, effective temperatures, bolometric and visual magnitudes, (U-B), (B-V), (V-R), (V-I), (V-J), (V-H), and (V-K) colors, and the luminosity function for the case of the Salpeter law. In addition to this, integrated magnitudes and colors at several characteristic points are also presented together with the mass of the remnant star when appropriate. The main characteristic that makes this set of isochrones very valuable is based on their extension in mass and chemical composition, besides the calculation of late stages of evolution, beyond the red giant tip till the white dwarf stage after the planetary nebula phase.

log(Age) Logarithm of the age yr M Current mass. It is usually increasing along the isochrone, but in the transition from the tip of the RGB to the ZAHB and from the tip of the AGB to the P-AGB phase. The mass is decreased in these transitions according to the effects of mass loss during the RGB phase, and the TP-AGB phase as described in section 3. Sun log(Teff) Logarithm of effective temperature K Mbol Bolometric magnitude mag V Absolute visual magnitude mag (U-B) (U-B) color index mag (B-V) (B-V) color index mag (V-R) (V-R) color index mag (V-I) (V-I) color index mag (V-J) (V-J) color index mag (V-H) (V-H) color index mag (V-K) (V-K) color index mag FLUM Luminosity function for the case of the Salpeter law --- Mwind Real value of the mass after mass loss by stellar wind for massive stars number=1 For massive stars the actual value of the mass is not given by the current mass along the isochrone, but it is derived taking into account mass loss by stellar wind as pointed out in section 2.2 of the text. Of course, for low and intermediate mass stars Mwind is not printed in z*.pst files, and its value is defined as zero in table* files. Only in the youngest isochrones, when massive stars are involved and mass loss by stellar wind is taken into account, the value of Mwind represents the actual mass associated to the corresponding luminosity and effective temperature. Sun z0004.pstPostscript files of table1 ready to print z001.pstPostscript files of table2 ready to print z004.pstPostscript files of table3 ready to print z008.pstPostscript files of table4 ready to print z02.pstPostscript files of table5 ready to print z05.pstPostscript files of table6 ready to print Patricia Bauer CDS 1994Mar21 J_A+AS_106_275.xml