Theoretical isochrones from models with new radiative opacities

Details Theoretical isochrones from models with new radiative opacities Theoretical isochrones from models with new radiative opacities

Aug 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994a%26as..106..275b&link_type=abstract

Astronomy and Astrophysics Suppl. 106, 275-302 (1994)

Astronomy and Astrophysics

Astrophysics

1250

Stars: Evolution, Interiors, Fundamental Parameters, Hr Diagram

Scientific paper

In this paper 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.

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