What we do and do not know about the s-process

Abstract

AGB stars are the source for the main component of the $s$-process. Here we discuss both the properties which are reasonably well known and those which still suffer from substantial uncertainties. In the former case, we are fairly sure that the $s$-process contribution from AGB stars comes from masses between about 1 and 3 $\msun$, and the dominant neutron source is the ${}^{13}$C$(\alpha$,n)${}^{16}$O reaction. In the latter category remains the formation mechanism for the ${}^{13}$C-pocket. Attempts at including rotation seem to inhibit neutron capture reactions. Explaining the observations seems to require a spread in the size of the ${}^{13}$C-pocket so some stochastic process, such as rotation, must be involved.

To be published in Nuclear Physics A; Invited Review for "Nuclei in the Cosmos VIII", Vancouver, July 2004

References in corpus (6)

• Galactic Evolution of Sr, Y, Zr: A Multiplicity of Nucleosynthetic Processes
• Nucleosynthesis and mixing on the Asymptotic Giant Branch. III. Predicted and observed s-process abundances
• Galactic chemical evolution of heavy elements: from Barium to Europium
• The s-Process in Rotating Asymptotic Giant Branch Stars
• More lead stars
• Lead: Asymptotic Giant Branch production and Galactic Chemical Evolution

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• Nucleosynthesis in helium-enriched asymptotic giant branch models: Implications for Heavy Element Enrichment in Omega Centauri
• Stellar laboratories III. New Ba V, Ba VI, and Ba VII oscillator strengths and the barium abundance in the hot white dwarfs G191-B2B and RE0503-289
• Stellar laboratories IV. New Ga IV, Ga V, and Ga VI oscillator strengths and the gallium abundance in the hot white dwarfs G191-B2B and RE0503-289
• Abundances on the Main Sequence of Omega Centauri