Low-Mass Binary Induced Outflows from Asymptotic Giant Branch Stars

By J. Nordhaus, Eric G. Blackman. 2006

194 citations recorded by the source corpus.

A significant fraction of planetary nebulae (PNe) and protoplanetary nebulae (PPNe) exhibit aspherical, axisymmetric structures, many of which are highly collimated. The origin of these structures is not entirely understood, however, recent evidence suggests that many observed PNe harbour binary systems, which may play a role in their shaping. In an effort to understand how binaries may produce such asymmetries, we study the effect of low-mass (<0.3M ⊙ ) companions (planets, brown dwarfs and low-mass main-sequence stars) embedded into the envelope of a 3.0-M ⊙ star during three epochs of its evolution [red giant branch, asymptotic giant branch (AGB), interpulse AGB]. We find that common envelope evolution can lead to three qualitatively different consequences: (i) direct ejection of envelope material resulting in a predominately equatorial outflow, (ii) spin-up of the envelope resulting in the possibility of powering an explosive dynamo-driven jet and (iii) tidal shredding of the companion into a disc which facilitates a disc-driven jet. We study how these features depend on the secondary's mass and discuss observational consequences.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/19529b5d98f66f4d71bea3b4dbedf3ea594e1abf

How researchers see this paper

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In Astronomy and Astrophysics

1. Robert G. Izzard
2. O. De Marco
3. Stan Woosley
4. A. Mustill
5. N. Soker
6. Eva Villaver
7. A. Kashi
8. Michela Mapelli

Citations in the corpus

• Dawes Review 6: The Impact of Companions on Stellar Evolution (2016, background): “It is not clear how these interactions alter the evolution of the stars (Soker, 1998b; Nelemans & Tauris, 1998; Nordhaus & Blackman, 2006; Staff et al., 2016b).”
• A circumbinary disc in the final stages of common envelope and the core-degenerate scenario for Type Ia supernovae (2011, methodology): “For our typical giant structure we approximate the AGB envelope structures from the models of Nordhaus & Blackman (2006), Tauris & Dewi (2001), and Soker (1992), that are qualitatively similar.”
• Pulsational Pair-instability Supernovae (2016, background): “If so, a substantial fraction of the primary’s envelope might be ejected in the plane of the orbit (e.g. Nordhaus & Blackman 2006; Morris & Podsiadlowski 2009; Smith 2011) just before the pulses begin.”
• FORETELLINGS OF RAGNARÖK: WORLD-ENGULFING ASYMPTOTIC GIANTS AND THE INHERITANCE OF WHITE DWARFS (2012, background): “Loss of orbital energy is very fast and the time-scale can be as short as weeks (Nordhaus & Blackman 2006).”