G. Bertelli

Scaled solar tracks and isochrones in a large region of the Z-Y plane I. From the ZAMS to the TP-AGB end for 0.15-2.5 M stars

Context. In many astrophysical contexts, the helium content of stars may differ significantly from those usually assumed in evolution- ary calculations. Aims. In order to improve upon this situation, we have computed tracks and isochrones in the range of initial masses 0.15−20 Mfor a grid of 39 chemical compositions with the metal content Z between 0.0001 and 0.070 and helium content Y between 0.23 and 0.46. Methods. The Padova stellar evolution code has been implemented with updated physics. New synthetic TP-AGB models allow the extension of stellar models and isochrones until the end of the thermal pulses along the AGB. Software tools for the bidimensional interpolation (in Y and Z) of the tracks have been tuned. Results. This first paper presents tracks for low mass stars (from 0.15 to 2.5 M� ) with scaled-solar abundances and the corresponding isochrones from very old ages down to about 1 Gyr. Conclusions. Tracks and isochrones are made available in tabular form for the adopted grid of chemical compositions in the plane Z-Y. As soon as possible an interactive web interface will allow users to obtain isochrones of any chemical composition and also simulated stellar populations with different Y(Z) helium-to-metal enrichment laws.

Scaled solar tracks and isochrones in a large region of the Z-Y plane. II. From 2.5 to 20 solar masses

We extend our theoretical computations for low-mass stars to intermediate-mass and massive stars, for which few databases exist in the literature. Evolutionary tracks and isochrones are computed for initial masses

Kinematics and stellar content of the Milky Way populations toward the North Galactic Pole

2.50{-}20~M_{odot}

Clues to the Evolution of the Carina Dwarf Spheroidal Galaxy from the Color Distribution of its Red Giant Stars

for a grid of 37 chemical compositions with metal content Z between 0.0001 and 0.070 and helium content Y between 0.23 and 0.40 to enable users to obtain isochrones for ages as young as about 10 7 years and to simulate stellar populations with different helium-to-metal enrichment laws. The Padova stellar evolution code is identical to that used in the first paper of this series. Synthetic TP-AGB models allow stellar tracks and isochrones to be extended until the end of the thermal pulses along the AGB. We provide software tools for the bidimensional interpolation (in Y and Z ) of the isochronesu2029from very old ages down to about 10 7 xa0years. This lower limit depends on chemical composition. The extension of the blue loops and the instability strip of Cepheid stars are compared and the Cepheid mass-discrepancy is discussed. The location of red supergiants in the H-R diagram is in good agreement with the evolutionary tracks for masses from 10 to

On the effect of helium enhancement on bolometric corrections and Teff-colour relations

20~M_{odot}

Thick disk kinematics from RAVE and the solar motion

. Tracks and isochrones are available in tabular form for the adopted grid of chemical compositions in the extended plane

On the instability strip of the Cepheid stars

Z-Y

On the mass discrepancy of the Cepheid stars

in three photometric systems. An interactive web interface allows users to obtain isochrones of any chemical composition inside the provided

Setting the clock of stellar models

Z-Y

Dissipative phenomena in extended-body interactions - I. Methods: Dwarf galaxies of the Local Group and their synthetic CMDs

range and also to simulate stellar populations with different