Some globular clusters host multiple stellar populations with different chemical abundance patterns. This is particularly true for ω Centauri, which shows clear evidence of a He-enriched sub-population characterized by a helium abundance as high as Y= 0.4. We present a whole and consistent set of evolutionary tracks from the ZAMS to the white dwarf stage appropriate for the study of the formation and evolution of white dwarfs resulting from the evolution of helium-rich progenitors. The final mass of the remnants, the role of overshooting during the thermally-pulsing phase, and the cooling of the resulting white dwarfs differ markedly from the evolutionary predictions of progenitor stars with standard initial helium abundance. For the range of initial masses explored in this paper, the final mass of the helium-rich progenitors is markedly larger than the final mass expected from progenitors with the usual helium abundance. Also, progenitors with initial mass smaller than M* ≈ 0.65 Msun evolve directly into He-core white dwarfs in less than 14 Gyr, and for larger progenitor masses the evolution of the resulting low-mass C-O white dwarfs is dominated by residual nuclear burning. He-core white dwarfs evolve faster than their counterparts coming from standard progenitors. In contrast with what occurs for white dwarfs resulting from progenitors with the standard helium abundance, the impact of residual burning on the cooling time of white dwarfs is not affected by the occurrence of overshooting during the thermally-pulsing phase of progenitor stars.
Althaus, L. G., De Gerónimo, F. C., Córsico, A. H., Torres, S., & García-Berro, E. 2017 A&A, to be published (arXiv:1611.06191)
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