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Nucleosynthesis in stars: The Origin of the Heaviest Elements

Published online by Cambridge University Press:  30 December 2019

Amanda I. Karakas Open the ORCID record for Amanda I. Karakas [Opens in a new window]
Amanda I. Karakas*
Affiliation:
Monash Centre for Astrophysics, School of Physics & Astronomy, Monash University, VIC 3800, Australia email: amanda.karakas@monash.edu
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Abstract

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The chemical evolution of the Universe is governed by the nucleosynthesis contribution from stars, which in turn is determined primarily by the initial stellar mass. The heaviest elements are primarily produced through neutron capture nucleosynthesis. Two main neutron capture processes identified are the slow and rapid neutron capture processes (s and r processes, respectively). The sites of the r and s-process are discussed, along with recent progress and their associated uncertainties. This review is mostly focused on the s-process which occurs in low and intermediate-mass stars which have masses up to about 8 solar masses (M⊙). We also discuss the intermediate-neutron capture process (or i-process), which may occur in AGB stars, accreting white dwarfs, and massive stars. The contribution of the i-process to the chemical evolution of elements in galaxies is as yet uncertain.

Keywords

nuclear reactionsnucleosynthesisabundancesstars: AGB and post-AGBgalaxies: abundances
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. 79 - 88
Copyright
© International Astronomical Union 2019 

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