2018MNRAS.480.1547L

We explore the evolution of hydrogen-rich and hydrogen-deficient white dwarf stars with masses between 1.012 and 1.307 M_☉, and initial metallicity of Z = 0.02. These sequences are the result of main-sequence stars with masses between 8.8 and 11.8 M_☉. The simulations were performed with MESA (Modules for Experiments in Stellar Astrophysics), starting at the zero-age main sequence, through thermally pulsing and mass-loss phases, ending at the white dwarf cooling sequence. We present reliable chemical profiles for the whole mass range considered, covering the different expected central compositions (i.e. C/O, O/Ne and Ne/O/Mg) and its dependence on the stellar mass. In addition, we present detailed chemical profiles of hybrid C/O-O/Ne core white dwarfs, found in the mass range between 1.024 and 1.15 M_☉. We present the initial-to-final mass relation, the mass-radius relation and cooling times considering the effects of atmosphere and core composition.