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 seque...
| Autores: | , , , , |
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| Formato: | artículo |
| Estado: | Versión publicada |
| Fecha de publicación: | 2005 |
| País: | Argentina |
| Recursos: | Consejo Nacional de Investigaciones Científicas y Técnicas |
| Repositorio: | CONICET Digital (CONICET) |
| Idioma: | inglés |
| OAI Identifier: | oai:ri.conicet.gov.ar:11336/38393 |
| Acesso em linha: | http://hdl.handle.net/11336/38393 |
| Access Level: | acceso abierto |
| Palavra-chave: | Evolution of stars Abundances AGB stars Interior stars White dwarfs Oscillations https://purl.org/becyt/ford/1.3 https://purl.org/becyt/ford/1 |
| Resumo: | 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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