S-process Nucleosynthesis in SAGB Stars

H H B Lau, Carolyn Doherty, Pilar Gil-Pons, John Charles Lattanzio

Research output: Chapter in Book/Report/Conference proceedingConference PaperResearch

Abstract

Super asymptotic giant branch (SAGB) stars, in a mass range between 5 and 11 M, have a similar evolution to high-mass AGB stars but are hot enough to ignite carbon in their cores non-degenerately during the early AGB phase. However, they could have a different nucleosynthesis signature because of the higher temperature at the bottom of intershell convective zone. In particular, 22Ne is the major source of neutrons. We have used the new Monash nucleosynthesis code MONTAGE to compute yields of 475 different isotopes, including s-process elements. We find 22Ne is the major source of neutrons and the 13C contribution is not significant. Moreover, the reaction rate of the triple-alpha reaction and 12C(α, γ)16O is critical to determine the nucleosynthesis of SAGB stars, particularly the heavy s-process isotopes and Pb.
Original languageEnglish
Title of host publicationWhy Galaxies Care about AGB Stars II: Shining Examples and Common Inhabitants
Subtitle of host publicationProceedings of a conference held at University Campus, Vienna, Austria 16-20 August 2010
EditorsF Kerschbaum, T Lebzelter, R F Wing
Place of PublicationSan Francisco CA USA
PublisherAstronomical Society of the Pacific
Pages45-50
Number of pages6
Volume445
Edition1
Publication statusPublished - 2011

Publication series

NameAstronomical Society of the Pacific Conference Series
PublisherAstronomical Society of the Pacific
Number1
Volume445

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