Evolutionary tracks for helium-core white dwarf stars resulting from progenitor stars with Z=0.02 Details are given in Althaus, Serenelli & Benvenuto et al. 2001, MNRAS, 323, 471. Each file refers to a specific evolutionary sequence characterized by a given stellar mass. For instance, t0169.dat stands for 0.169 (solar masses) He-core white dwarf models. In each file it is listed from left to right log of photon luminosity (in solar units), log of effective temperature (K), log of central temperature (in millon degree), log central density, age (in yr counted from the end of mass loss, see below), log stellar radius (cm), log surface gravity, log H-burning luminosity (in solar unit), abundance by mass of hydrogen below the photosphere, log of the H outer mass fraction.

Note: The end of mass loss episode during the pre-wd evolution is taken to be at Teff= 5000K for 0.406, 0.360, 0.327, 0.292 and 0.242Msun models and Teff= 10000K for 0.196 and 0.169Msun models.

Evolution is followed in a self-consistent way with the predictions of detailed nongray model atmospheres, time-dependent element diffusion and the history of the white dwarf progenitor. We have followed the evolution of He WD models with stellar masses of 0.406, 0.360, 0.327, 0.292, 0.242, 0.196, 0.169M_sun. All of these models were evolved from the end of the mass-loss phase, during the pre-WD evolution, through the stages of hydrogen shell flashes (when they take place) down to very advanced stages of evolution.