We explore the evolution of hydrogen-rich and hydrogen-deficient white dwarf stars with masses between 1.012 and 1.307 M _ { \odot } , 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 _ { \odot } .
The simulations were performed with MESA , starting at the zero-age main sequence , through thermally pulsing and mass-loss phases , ending at the white dwarfs 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 with 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 _ { \odot } .
We present the initial-to-final mass relation , mass-radius relation , and cooling times considering the effects of atmosphere and core composition .