The formation of DA white dwarfs with thin hydrogen envelopes
We study the formation and evolution of DA white dwarfs, the progenitors of which have experienced a late thermal pulse (LTP) shortly after the departure from the thermally pulsing AGB. To this end, we compute the complete evolution of an initially 2.7 M⊙ star all the way from the zero-age main sequ...
| Autores: | , , , , |
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| Tipo de recurso: | artículo |
| Estado: | Versión publicada |
| Fecha de publicación: | 2005 |
| País: | Argentina |
| Institución: | Universidad Nacional de La Plata |
| Repositorio: | SEDICI (UNLP) |
| Idioma: | inglés |
| OAI Identifier: | oai:sedici.unlp.edu.ar:10915/83410 |
| Acceso en línea: | http://sedici.unlp.edu.ar/handle/10915/83410 |
| Access Level: | acceso abierto |
| Palabra clave: | Ciencias Astronómicas Stars: abundances Stars: AGB stars: interiors Stars: evolution Stars: oscillations Stars: white dwarfs |
| Sumario: | We study the formation and evolution of DA white dwarfs, the progenitors of which have experienced a late thermal pulse (LTP) shortly after the departure from the thermally pulsing AGB. To this end, we compute the complete evolution of an initially 2.7 M⊙ star all the way from the zero-age main sequence to the white dwarf stage. We find that most of the original H-rich material of the post-AGB remnant is burnt during the post-LTP evolution, with the result that, at entering its white dwarf cooling track, the remaining H envelope becomes 10-6 M⊙ in agreement with asteroseismological inferences for some ZZ Ceti stars. |
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