Abstract
The slow neutron-capture process (s process) contributes to the production of roughly half of the elements heavier than iron. The main component of the s process takes place in the late phases (AGB phase) of low-mass stars and is the topic of most reviews on the s process. This review thus focuses on the weak s process taking place in massive stars with a special emphasis on the key role of rotation as well as key stellar and nuclear uncertainties. While the weak s process production at solar metallicity is limited to the first peak (Sr), rotation-induced mixing boosts this production at low metallicities to the second peak (Ba) and in extreme cases to the third peak (Pb). Rotation-boosted s process also opens the door to an enhanced production of p nuclei compared to classical non-rotating massive star model predictions.
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Acknowledgements
RH acknowledges current and past members of the Geneva stellar evolution group and Basel theoretical Physics group and thanks them for many years of fruitful collaboration. RH also acknowledges support from the World Premier International Research Centre Initiative (WPI Initiative), MEXT, Japan, and the IReNA AccelNet Network of Networks (National Science Foundation, Grant No. OISE-1927130). This article is based upon work from the ChETEC COST Action (CA16117) and the European Union’s Horizon 2020 research and innovation programme (ChETEC-INFRA, Grant No. 101008324).
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Hirschi, R. (2023). Slow Neutron-Capture Process in Evolved Stars. In: Tanihata, I., Toki, H., Kajino, T. (eds) Handbook of Nuclear Physics . Springer, Singapore. https://doi.org/10.1007/978-981-15-8818-1_118-1
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