Abstract We study the full evolution of a 1. 313 M_ white dwarf star that descended from a 9 M_ main-sequence progenitor with an initial metallicity of Z=0. 02. Using MESA r24. 08. 01, we calculate its entire evolution from pre-ZAMS to the WD cooling curve, including both the evolution through 139 thermal pulses and the post-AGB phase. The resulting remnant is an ultramassive H-deficient WD, for which the composition, in mass fraction, is 47. 7% 16O, 39. 7% 20Ne, 4. 2% 24Mg, 3. 3% 23Na and 0. 386% ^12 C – corresponding to a total mass of 5 10^-3 \, M_ of C –, surrounded by a 1. 5 10^-5 M_ He layer. We also investigate the effects of fully suppressing the TP-SAGB stage by adopting a high mass-loss rate only after the second dredge-up, and find only minor differences in the final mass and composition. In addition, we calculate models with and without phase separation during the WD stage, estimating a cooling delay of only 16 Myr. This is the first ultramassive white dwarf sequence for which both the TP-SAGB and post-AGB stages are calculated and, to our knowledge, the most massive WD model from complete evolution for which cooling times and detailed abundance profiles are published.
Antonini et al. (Tue,) studied this question.