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We explore the evolution of hydrogen-rich and hydrogen-deficient white dwarf stars with masses between 1.012 and 1.307M , and initial metallicity of Z = 0.02. These sequences are the result ofmain-sequence stars with masses between 8.8 and 11.8M . The simulations were performed with MESA (Modules for Experiments in Stellar Astrophysics), starting at the zeroage 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 corewhite dwarfs, found in themass range between 1.024 and 1.15M .We present the initial-to-final mass relation, the mass–radius relation and cooling times considering the effects of atmosphere and core composition.
Lauffer et al. (Wed,) studied this question.