2016ApJ...823..158C

Because of the large neutron excess of ²²Ne, sedimentation of this isotope occurs rapidly in the interior of white dwarfs. This process releases an additional amount of energy, thus delaying the cooling times of the white dwarf. This influences the ages of different stellar populations derived using white dwarf cosmochronology. Furthermore, the overabundance of ²²Ne in the inner regions of the star modifies the Brunt-Vaisala frequency, thus altering the pulsational properties of these stars. In this work we discuss the impact of ²²Ne sedimentation in white dwarfs resulting from solar metallicity progenitors (Z=0.02). We performed evolutionary calculations of white dwarfs with masses of 0.528, 0.576, 0.657, and 0.833 {M}_☉ derived from full evolutionary computations of their progenitor stars, starting at the zero-age main sequence all the way through the central hydrogen and helium burning, the thermally pulsing asymptotic giant branch (AGB), and post-AGB phases. Our computations show that at low luminosities ( log(L/L_☉)\lesssim -4.25 ), ²²Ne sedimentation delays the cooling of white dwarfs with solar metallicity progenitors by about 1 Gyr. Additionally, we studied the consequences of ²²Ne sedimentation on the pulsational properties of ZZ Ceti white dwarfs. We find that ²²Ne sedimentation induces differences in the periods of these stars larger than the present observational uncertainties, particularly in more massive white dwarfs.