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Dynamics, temperature, chemistry, and dust: Ingredients for a self-consistent AGB wind

Published online by Cambridge University Press:  30 December 2019

J. Boulangier Open the ORCID record for J. Boulangier [Opens in a new window] ,
D. Gobrecht  and
L. Decin
J. Boulangier
Affiliation:
Institute of Astronomy, KU Leuven, Celestijnenlaan 200D, 3001 Leuven, Belgium email: [email protected]
D. Gobrecht
Affiliation:
Institute of Astronomy, KU Leuven, Celestijnenlaan 200D, 3001 Leuven, Belgium email: [email protected]
L. Decin
Affiliation:
Institute of Astronomy, KU Leuven, Celestijnenlaan 200D, 3001 Leuven, Belgium email: [email protected] University of Leeds, School of Chemistry, Leeds LS2 9JT, United Kingdom
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Abstract

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Understanding Asymptotic Giant Branch (AGB) stars is important as they play a vital role in the chemical life cycle of galaxies. AGB stars are in a phase of their life time where they have almost ran out of fuel and are losing vast amounts of material to their surroundings, via stellar winds. As this is an evolutionary phase of low mass stars, almost all stars go through this phase making them one of the main contributors to the chemical enrichment of galaxies. It is therefore important to understand what kind of material is being lost by these stars, and how much and how fast. This work summarises the steps we have taken towards developing a self-consistent AGB wind model. We improve on current models by firstly coupling chemical and hydrodynamical evolution, and secondly by upgrading the nucleation theory framework to investigate the creation of TiO2, SiO, MgO, and Al2O3 clusters.

Keywords

stars: AGB and post-AGBstars: windsoutflowshydrodynamicsastrochemistrymethods: numerical
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 14 , Symposium S343: Why Galaxies Care About AGB Stars: A Continuing Challenge through Cosmic Time , August 2018 , pp. 129 - 133
Copyright
© International Astronomical Union 2019 

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