Volume 451, Number 1, May III 2006
|Page(s)||147 - 155|
|Section||Stellar structure and evolution|
|Published online||25 April 2006|
DQ white-dwarf stars with low C abundance: possible progenitors
Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata, Paseo del Bosque, s/n, (1900) La Plata, Argentina Instituto de Astrofísica La Plata, IALP, CONICET e-mail: [cscoccola;althaus;acorsico]@fcaglp.unlp.edu.ar
2 Institute for Advanced Study, School of Natural Sciences, Einstein Drive, Princeton, NJ, 08540, USA e-mail: firstname.lastname@example.org
3 Observatorio Astronómico, Universidad Nacional de Córdoba, Laprida 854, (5000) Córdoba, Argentina e-mail: email@example.com
Accepted: 1 December 2005
Aims.The present paper focuses on the evolution of hydrogen-deficient white dwarfs with the aim of exploring the consequences of different initial envelope structures on the carbon abundances expected in helium-rich, carbon-contaminated DQ white dwarfs. In particular, the evolutionary link between the DQs with low detected carbon abundances and the PG 1159, extreme horizontal branch, and helium-rich R Coronae Borealis (RCrB) stars is explored.
Methods.We present full evolutionary calculations that take a self-consistent treatment of element diffusion into account as well as expectations for the outer layer chemical stratification of progenitor stars upon entering the white dwarf regime.
Results.We find that PG 1159 stars cannot be related to any DQ white dwarfs with low C abundances. Instead, we suggest that the latter could constitute the progeny of the giant, helium-rich RCrB stars.
© ESO, 2006
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