Volume 507, Number 3, December I 2009
|Page(s)||1575 - 1583|
|Section||Stellar structure and evolution|
|Published online||01 October 2009|
Very low-mass white dwarfs with a C–O core
Physics Department “E. Fermi”, University of Pisa, largo B. Pontecorvo 3, 56127 Pisa, Italy e-mail: email@example.com
2 INFN, largo B. Pontecorvo 3, 56127 Pisa, Italy
3 INAF – Osservatorio Astronomico di Collurania, via Maggini, 64100 Teramo, Italy e-mail: firstname.lastname@example.org
Accepted: 9 September 2009
Context. The lower limit for the mass of white dwarfs (WDs) with a C-O core is commonly assumed to be roughly 0.5 . As a consequence, WDs of lower masses are usually identified as He-core remnants.
Aims. When the initial mass of the progenitor star is between 1.8 and 3 , which corresponds to the so-called red giant (RGB) phase transition, the mass of the H-exhausted core at the tip of the RGB is 0.3 < < 0.5. Prompted by this well known result of stellar evolution theory, we investigate the possibility to form C-O WDs with mass M < 0.5 .
Methods. The pre-WD evolution of stars was computed with initial mass of about 2.3 , undergoing anomalous mass-loss episodes during the RGB phase and leading to the formation of WDs with He-rich or CO-rich cores. The cooling sequences of the resulting WDs are also described.
Results. We show that the minimum mass for a C-O WD is about 0.33 , so that both He and C-O core WDs can exist in the mass range 0.33-0.5 . The models computed for the present paper provide the theoretical tools for indentifying the observational counterpart of very low-mass remnants with a C-O core among those commonly ascribed to the He-core WD population in the progressively growing sample of observed WDs of low mass. Moreover, we show that the central He-burning phase of the stripped progeny of the 2.3 star lasts longer and longer as the total mass decreases. In particular, the M = 0.33 model takes about 800 Myr to exhaust its central helium, which is more than three times longer than the value for the standard 2.3 star: it is, by far, the longest core-He burning lifetime. Finally, we find the occurrence of gravonuclear instabilities during the He-burning shell phase.
Key words: stars: evolution / stars: white dwarfs / stars: horizontal-branch / stars: interiors / stars: oscillations
© ESO, 2009
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