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Route towards complete 3D hydro-chemical simulations of companion-perturbed AGB outflows

Published online by Cambridge University Press:  30 November 2022

Silke Maes Open the ORCID record for Silke Maes [Opens in a new window] ,
Lionel Siess ,
Ward Homan ,
Jolien Malfait Open the ORCID record for Jolien Malfait [Opens in a new window] ,
Frederik De Ceuster ,
Thomas Ceulemans ,
Dion Donné ,
Mats Esseldeurs Open the ORCID record for Mats Esseldeurs [Opens in a new window]  and
Leen Decin
Silke Maes
Affiliation:
Instituut voor Sterrenkunde, KU Leuven, Celestijnenlaan 200D, 3001 Leuven, Belgium email: silke.maes@kuleuven.be
Lionel Siess
Affiliation:
Institut d’Astronomie et d’Astrophysique, Université Libre de Bruxelles (ULB), CP 226, 1050 Brussels, Belgium
Ward Homan
Affiliation:
Institut d’Astronomie et d’Astrophysique, Université Libre de Bruxelles (ULB), CP 226, 1050 Brussels, Belgium
Jolien Malfait
Affiliation:
Instituut voor Sterrenkunde, KU Leuven, Celestijnenlaan 200D, 3001 Leuven, Belgium email: silke.maes@kuleuven.be
Frederik De Ceuster
Affiliation:
Instituut voor Sterrenkunde, KU Leuven, Celestijnenlaan 200D, 3001 Leuven, Belgium email: silke.maes@kuleuven.be Department of Physics and Astronomy, University College London, Gower Place, London, WC1E 6BT, UK
Thomas Ceulemans
Affiliation:
Instituut voor Sterrenkunde, KU Leuven, Celestijnenlaan 200D, 3001 Leuven, Belgium email: silke.maes@kuleuven.be
Dion Donné
Affiliation:
Instituut voor Sterrenkunde, KU Leuven, Celestijnenlaan 200D, 3001 Leuven, Belgium email: silke.maes@kuleuven.be
Mats Esseldeurs
Affiliation:
Instituut voor Sterrenkunde, KU Leuven, Celestijnenlaan 200D, 3001 Leuven, Belgium email: silke.maes@kuleuven.be
Leen Decin
Affiliation:
Instituut voor Sterrenkunde, KU Leuven, Celestijnenlaan 200D, 3001 Leuven, Belgium email: silke.maes@kuleuven.be School of Chemistry, University of Leeds, Leeds LS2 9JT, UK
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Abstract

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Low- and intermediate mass stars experience a significant mass loss during the last phases of their evolution, which obscures them in a vast, dusty envelope. Although it has long been thought this envelope is generally spherically symmetric in shape, recent high-resolution observations find that most of these stars exhibit complex and asymmetrical morphologies, most likely resulting from binary interaction. In order to improve our understanding about these systems, theoretical studies are needed in the form of numerical simulations. Currently, a handful of simulations exist, albeit they mainly focus on the hydrodynamics of the outflow. Hence, we here present the pathway to more detailed and accurate modelling of companion-perturbed outflows with, by discussing the missing but crucial physical and chemical processes. With these state-of-the-art simulations we aim to make a direct comparison with observations to unveil the true identity on the embedded systems.

Keywords

Stars: AGBStars: winds, outflowsMethods: numerical
Type
Contributed Paper
Information
Proceedings of the International Astronomical Union , Volume 16 , Symposium S366: The Origin of Outflows in Evolved Stars , November 2020 , pp. 227 - 233
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Copyright
© The Author(s), 2022. Published by Cambridge University Press on behalf of International Astronomical Union

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