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The evolution of white dwarfs resulting from helium-enhanced , low-metallicity progenitor stars
| Content Provider | Semantic Scholar |
|---|---|
| Author | Althaus, Leandro G. Gerónimo, Francisco De Córsico, Alejandro H. Torres, Santiago Enrique Berro, García – |
| Copyright Year | 2016 |
| Abstract | Context. Some globular clusters host multiple stellar populations with di fferent chemical abundance patterns. This is particularly true for ω Centauri, which shows clear evidence of a helium-enriched sub-popula tion characterized by a helium abundance as high as Y = 0.4 Aims. We present a whole and consistent set of evolutionary tracks from the Z AMS 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. Methods. White dwarf sequences have been derived from progenitors with stellar mass ranging from 0.60 to 2 .0 M⊙ and for an initial helium abundance of Y = 0.4. Two values of metallicity have been adopted: Z = 0.001 andZ = 0.0005. Results. Different issues of the white dwarf evolution and their helium-rich progenitors have been explored. In particular, the final mass of the remnants, the role of overshooting during the thermally-pulsin g phase, and the cooling of the resulting white dwarfs differ markedly from the evolutionary predictions of progenitor stars with stan dard initial helium abundance. Finally, the pulsational properties of the resulting white dwarfs are also explored. Conclusions. We find that, 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 us ual helium abundance. We also find that progenitors with initial mass smaller than M ≃ 0.65M⊙ evolve directly into helium-core white dwarfs in less than 14 Gyr, and that fo r larger progenitor masses the evolution of the resulting low-mass carbon-oxygen white dwar fs is dominated by residual nuclear burning. For helium-core white dwarfs, we find that they evolve markedly faster than their counterp arts coming from standard progenitors. Also, in contrast with what occurs for white dwarfs resulting from progenitors with the stand ard helium abundance, the impact of residual burning on the cooling time of white dwarfs is not a ffected by the occurrence of overshooting during the thermally-pulsing ph ase of progenitor stars. |
| File Format | PDF HTM / HTML |
| Alternate Webpage(s) | http://upcommons.upc.edu/bitstream/handle/2117/101528/He40.pdf;jsessionid=DD2E89D88532023CBC50F240EC23ECC7?sequence=1 |
| Language | English |
| Access Restriction | Open |
| Subject Keyword | ABRA gene Computer cooling Cool - action DWARF Entity Name Part Qualifier - adopted Evolution Helium Large Oxygen Population Sid Meier's Alpha Centauri Small Stan (fan) Stars, Celestial Stellar (payment network) VHDL-AMS |
| Content Type | Text |
| Resource Type | Article |
