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Fig. 1


Evolutionary tracks of white dwarf models with M ~ 0.51−0.54 M on the log Teff − log g plane. Each panel corresponds to a different metallicity value (Z) of the white dwarf progenitors. For the case of Z = 0.0001 we include two additional sequences with masses M = 0.666 M and M = 0.738 M. Red thick segments on the tracks at log Teff ~ 4 correspond to DA white dwarf models having the dipole g1-mode destabilized mostly by the ε mechanism acting at the hydrogen burning shell. The violet thick segment in the case of the M = 0.535 M and Z = 0.0001 sequence corresponds to models with unstable low-order g-modes (g1 to g4) destabilized solely by the ε mechanism. The dashed green line indicates the theoretical red edge of the instability domain of pre-white-dwarfs with hydrogen-rich envelopes evolved from MZAMS ≥ 1.5 M with solar metallicity found by Maeda & Shibahashi (2014). The almost vertical dotted blue line corresponds to the empirical blue edge of the instability domain of ZZ Ceti stars reported by Gianninas et al. (2011).

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