AGB stars in binaries and their progeny

Jorissen, A.

doi:10.1017/s0074180900203380

Cited by 7 publications

(3 citation statements)

References 34 publications

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“…Finally, we would like to emphasize that one of our most important findings is that Asymptotic Giant Branch stars could indeed be found in binary systems, in agreement with the predictions of Jorissen (1999). The Super-Asymptotic Giant Branch star is the secondary of a binary system in our scenario 1.b, and should have an evolved (and possibly degenerate) companion.…”

Section: Discussionsupporting

confidence: 84%

“…Moreover, most of the developments in the field of binaries frequently disregarded the study of AGB stars, arguing that this phase is prematurely quenched in binary systems, due to significant mass loss in the evolution previous to the AGB phase. Important exceptions are the works of Jorissen (1999) and Smith et al (1996) who proposed the existence of AGB stars in binary systems and, more recently, Van Eck et al (2001), who found observational evidence of three AGB stars in binary systems.…”

Section: Introductionmentioning

confidence: 99%

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On the formation of Super-AGB stars in intermediate mass close binary systems

Gil‐Pons¹,

Garcı́a–Berro

2002

A&A

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Abstract. The evolution of a star of initial mass 9 M , and metallicity Z = 0.02 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 M , whereas in the second one the mass was assumed to be 1 M . 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 (q = 0.1) 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.

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Section: Discussionsupporting

confidence: 84%

Section: Introductionmentioning

confidence: 99%

On the formation of Super-AGB stars in intermediate mass close binary systems

Gil‐Pons¹,

Garcı́a–Berro

2002

A&A

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“…Traditionally considered as transition objects between M oxygen-rich and C carbon-rich stars on the AGB (Iben & Renzini 1983), they are classified in 2 categories: the intrinsic Tc-Rich S stars have a circumstellar envelope. The extrinsic Tc-poor S stars do not show any envelope, which is explained by a different evolutionary scenario involving a present white dwarf companion (Jorissen 1998;Jorissen & Knapp 1998). The giant star π 1 Gru is known to have a faint and far solar-type G0V companion (apparent visible magnitude of 10.9, angular distance of 2.71 from the primary, not changed since 1900) (Feast 1953), considered as having very little effect on the close circumstellar envelope (Mastrodemos & Morris 1998;Knapp et al 1999).…”

Section: General Characteristicsmentioning

confidence: 86%

A new analytical thin-dusty-shell model to interpret interferometric data

Cruzalèbes¹,

Sacuto²

2006

A&A

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High angular resolution techniques allow the determination of physical and geometrical parameters characterizing the circumstellar dusty environment of late-type stars. The resolution of the radiative transfer equation under the thin-shell approximation provides an analytical expression for the interferometric visibility profile, which can then be compared to simple ad-hoc geometrical models and to physical models based on radiative transfer. Using the DUSTY numerical code to calculate theoretical visibilities of the S star π 1 Gru, in agreement with spectrophotometric measurements from the near to the far infrared, we compared the validity of the output parameters found by the χ 2 least-square analysis of the visibility, given with the thin-shell model and with a simple disk+ring geometrical model of the envelope. The results are discussed in terms of fitting the shape of the intensity profile and of the number of free parameters to be considered.

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What Can We Learn from Post-AGB Chemical Studies on the AGB 3 RD Dredge-Up Phenomena?

Winckel

Reyniers

2001

Post-Agb Objects as a Phase of Stellar Evolution

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AGB stars in binaries and their progeny

Cited by 7 publications

References 34 publications

On the formation of Super-AGB stars in intermediate mass close binary systems

On the formation of Super-AGB stars in intermediate mass close binary systems

A new analytical thin-dusty-shell model to interpret interferometric data

What Can We Learn from Post-AGB Chemical Studies on the AGB 3 RD Dredge-Up Phenomena?

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