Abstract
The chemical evolution of galaxies is governed by the chemical yields from stars, especially from Asymptotic Giant Branch (AGB) stars. This underlines the importance of understanding how AGB stars produce their elements by obtaining accurate stellar nucleosynthetic yields. Although AGB nucleosynthesis has general validity, critical uncertainties (such as the treatment of convective-driven mixing processes and mass loss) exist in current stellar models. Observations from post-Asymptotic Giant Branch (post-AGB) stars serve as excellent tools to quantify the strongest discrepancies, and eliminate crucial uncertainties that hamper stellar modelling. Our recent studies of post-AGB stars have shown an intriguing chemical diversity that ranges from stars that are extremely enriched in carbon and s-process elements to the discovery of the first post-AGB star with no traces of carbon nor s-process elements. Additionally, AGB nucleosynthesis is significantly affected by a binary companion. These results reflect the complexity that surrounds the element production in AGB stars. In this review, I will briefly present the intriguing chemical diversity observed in post-AGB stars and its implications on element/isotope production in AGB stars and stellar nucleosynthetic yields.
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Acknowledgements
The author acknowledges all the brilliant astronomers who have contributed to the field of AGB and post-AGB stars. She acknowledges the support of the Australian Research Council (ARC), Discovery Early Career Research Award (DECRA) Grant (95213534). She also acknowledges the funding provided by the Indian Institute of Astrophysics (IIA), Bangalore that enabled her to attend the conference, “Celebration of 150 Years of Periodic Table: Chemical Elements in the Universe”, which was held at IIA, Bengaluru, India from 16/12/2019 to 19/12/2019.
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This article is part of the Topical Collection: Chemical Elements in the Universe: Origin and Evolution.
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Kamath, D. Post-AGB stars as tracers of the origin of elements in the universe. J Astrophys Astron 41, 42 (2020). https://doi.org/10.1007/s12036-020-09665-4
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DOI: https://doi.org/10.1007/s12036-020-09665-4