SIMULATING THE COMMON ENVELOPE PHASE OF A RED GIANT USING SMOOTHED-PARTICLE HYDRODYNAMICS AND UNIFORM-GRID CODES
- Department of Astrophysics, American Museum of Natural History, New York, NY (United States)
- Department of Physics and Astronomy, Macquarie University, Sydney, NSW (Australia)
- Computational Computer Science Division, Los Alamos National Laboratory, Los Alamos, NM (United States)
- Department of Physics and Astronomy, University of Victoria, Victoria, BC (Canada)
- Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, Palo Alto, CA (United States)
- Department of Astronomy, Columbia University, New York, NY (United States)
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{sub Sun} and a companion star of mass ranging from 0.9 down to 0.1 M{sub Sun }. 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{sub Sun }, 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.
- OSTI ID:
- 22004334
- Journal Information:
- Astrophysical Journal, Vol. 744, Issue 1; Other Information: Country of input: International Atomic Energy Agency (IAEA); ISSN 0004-637X
- Country of Publication:
- United States
- Language:
- English
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