SIMULATING THE COMMON ENVELOPE PHASE OF A RED GIANT USING SMOOTHED-PARTICLE HYDRODYNAMICS AND UNIFORM-GRID CODES
By Jean-Claude Passy, O. De Marco, Chris L. Fryer, Falk Herwig, S. Diehl, Jeffrey S. Oishi, M. Mac Low, Greg L. Bryan, Gabriel Rockefeller. 2011
171 citations recorded by the source corpus.
We use three-dimensional hydrodynamical simulations to study the rapid infall phase of the common envelope (CE) interaction of a red giant branch star of mass equal to 0.88 M☉ and a companion star of mass ranging from 0.9 down to 0.1 M☉. We first compare the results obtained using two different numerical techniques with different resolutions, and find very good agreement overall. We then compare the outcomes of those simulations with observed systems thought to have gone through a CE. The simulations fail to reproduce those systems in the sense that most of the envelope of the donor remains bound at the end of the simulations and the final orbital separations between the donor's remnant and the companion, ranging from 26.8 down to 5.9 R☉, are larger than the ones observed. We suggest that this discrepancy vouches for recombination playing an essential role in the ejection of the envelope and/or significant shrinkage of the orbit happening in the subsequent phase.
Subfields: Astronomy and Astrophysics, Instrumentation
View Paper: https://www.semanticscholar.org/paper/856bd92d10d73815383a7fe89b1dc949c6e0050c
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In Astronomy and Astrophysics
- John H. Wise
- M. Norman
- Tom Abel
- Christoph Federrath
- P. Hopkins
- Matthew J. Turk
- Brian W. O'Shea
- Ralf Klessen
In Instrumentation
- John H. Wise
- Tom Abel
- M. Norman
- Robert G. Izzard
- Renyue Cen
- N. Langer
- Matthew J. Turk
- Brian W. O'Shea
Citations in the corpus
- AN AMR STUDY OF THE COMMON-ENVELOPE PHASE OF BINARY EVOLUTION (2011, unknown): “A definitive understanding of the CE phase requires computationally intensive hydrodynamical simulations of which a number of recent studies have been carried out (e.g., Ricker & Taam 2008; Taam & Ricker 2010; Passy et al. 2012).”
- ENZO: AN ADAPTIVE MESH REFINEMENT CODE FOR ASTROPHYSICS (2013, methodology): “Finally, Passy et al. (2012) show the results of comparing Enzo in its non-AMR mode to a smoothed-particle hydrodynamics code, SNSPH, in the context of common-envelope binary stellar interactions.”
- Theoretical uncertainties of the Type Ia supernova rate (2014, background): “Because of the short timescale of the CE phase (e.g. Passy et al. 2012), we assume in our standard model that no mass is accreted by the companion star (Table 1).”
- Formation of millisecond pulsars with CO white dwarf companions – II. Accretion, spin-up, true ages and comparison to MSPs with He white dwarf companions (2012, background): “The total duration of the CE-phase itself is probably so short (< 103 yr, e.g. Podsiadlowski 2001; Passy et al. 2012; Ivanova et al. 2012) that no substantial accretion onto the neutron star is possible with respect to changing its rotational dynamics – even if the envelope of the donor star is not…”