Volume 396, Number 2, December III 2002
|Page(s)||589 - 598|
|Section||Interstellar and circumstellar matter|
|Published online||03 December 2002|
On the formation of Super-AGB stars in intermediate mass close binary systems
Departament de Física Aplicada, Universitat Politècnica de Catalunya, c/Jordi Girona s/n, Módul B-4, Campus Nord, 08034 Barcelona, Spain e-mail: pilar, email@example.com
2 Institute for Space Studies of Catalonia, c/Gran Capitá 2–4, Edif. Nexus 104, 08034 Barcelona, Spain
Corresponding author: E. García–Berro, firstname.lastname@example.org
Accepted: 10 September 2002
The evolution of a star of initial mass 9 , and metallicity in a Close Binary System (CBS) is followed in the presence of different mass companions in order to study their influence on the final evolutionary stages and, in particular, on the structure and composition of the remnant components. In order to do that, we study two extreme cases. In the first one the mass of the secondary is 8 , whereas in the second one the mass was assumed to be 1 . For the first of those cases we have also explored the possible outcomes of both conservative and non-conservative mass-loss episodes. During the first mass transfer episode, several differences arise between the models. The system with the more extreme mass ratio () is not able to survive the first Roche lobe overflow (RLOF) as a binary, but instead, spiral-in of the secondary onto the envelope of the primary star is most likely. The system formed by two stars of comparable mass undergoes two mass transfer episodes in which the primary is the donor. We have performed two sets of calculations corresponding to this case in order to account for conservative and non-conservative mass transfer during the first mass loss episode. One of our main results is that for the non-conservative case the secondary becomes a Super–AGB star in a binary system. Such a star undergoes a final dredge-up episode, similar to that of a single star of comparable mass. The primary components do not undergo a Super–AGB phase, but instead a carbon-oxygen white dwarf is formed in both cases (conservative and non-conservative), before reversal mass transfer occurs. However, given the extreme mass ratios at this stage between the components of the binary system, especially for the conservative case, the possibility of merger episodes remains likely. We also discuss the presumable final outcomes of the system and possible observational counterparts.
Key words: stars: evolution / stars: binaries: general / stars: AGB and post-AGB / stars: white dwarfs
© ESO, 2002
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