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Mass transfer in AGB binaries - uncovering a new evolution channel by 3D radiation-hydrodynamic simulations

Published online by Cambridge University Press:  30 November 2022

Zhuo Chen Open the ORCID record for Zhuo Chen [Opens in a new window] ,
Natalia Ivanova Open the ORCID record for Natalia Ivanova [Opens in a new window]  and
Jonathan Carroll-Nellenback
Zhuo Chen
Affiliation:
Department of Astronomy, Tsinghua University Beijing 100084, China email: [email protected]
Natalia Ivanova
Affiliation:
Department of Physics, University of Alberta Edmonton, AB T6G 2E1, Canada
Jonathan Carroll-Nellenback
Affiliation:
Department of Physics and Astronomy, University of Rochester Rochester, NY 14627, USA
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Abstract

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The origin of chemically peculiar stars and nonzero eccentricity in evolved close binaries have been long-standing problems in binary stellar evolution. Answers to these questions may trace back to an intense mass transfer during the asymptotic-giant-branch (AGB) binary phase. We use AstroBEAR to solve the 3D radiation hydrodynamic equations and calculate the mass transfer rate in AGB binaries that undergo the wind-Roche-lobe overflow or Bondi-Hoyle-Lyttleton (BHL) accretion. One of the goals of this work is to illustrate the transition from the wind- Roche-lobe overflow to BHL accretion. Both circumbinary disks and spiral structure outflows can appear in the simulations. As a result of enhanced mass transfer and angular momentum transfer, some AGB binaries may undergo orbit shrinkage, and some will expand. The high mass transfer efficiency is closely related to the presence of the circumbinary disks.

Keywords

Asymptotic giant branchSymbiotic binary starsHydrodynamics
Type
Contributed Paper
Information
Proceedings of the International Astronomical Union , Volume 16 , Symposium S366: The Origin of Outflows in Evolved Stars , November 2020 , pp. 222 - 226
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Copyright
© The Author(s), 2022. Published by Cambridge University Press on behalf of International Astronomical Union

References

Balbus, S. A. and Hawley, J. F. 1991, ApJ, 376, 214 CrossRefGoogle Scholar
Bondi, H. and Hoyle, F. 1944, MNRAS, 104, 273 CrossRefGoogle Scholar
Podsiadlowski, Ph. and Mohamed, S. 2007, Baltic Astronomy, 16, 26 Google Scholar
Chen, Z., Blackman, E. G., Nordhaus, J., Frank, A., and Carroll-Nellenback, J. 2018, MNRAS, 473, 747 CrossRefGoogle Scholar
Chen, Z., Ivanova, N., and Carroll-Nellenback, J. 2020, ApJ, 892, 110 CrossRefGoogle Scholar
Ertel, S., Kamath, D., Hillen, M. et al 2019, AJ, 157, 110 CrossRefGoogle Scholar
Höfner, S. and Freytag, B. 2019, A&A, 623, A158 Google Scholar
Kervella, P., Montargès, M., Lagadec, E., et al. 2015, A&A, 578, A77 Google Scholar
Mohamed, S. and Podsiadlowski, Ph. 2012, Baltic Astronomy, 21, 88 Google Scholar
Muñoz, D., Miranda, R. and Lai, D. 2019, ApJ, 871, 84 CrossRefGoogle Scholar
Shakura, N. I. and Sunyaev, R. A. 1973, A&A, 500, 33 Google Scholar