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The slow-neutron capture process in low-metallicity asymptotic giant branch stars

Published online by Cambridge University Press:  09 March 2010

Amanda I. Karakas ,
Maria Lugaro  and
Simon W. Campbell
Amanda I. Karakas
Affiliation:
Mount Stromlo Observatory, Australian National University, Weston Creek ACT 2611, Australia email: akarakas@mso.anu.edu.au
Maria Lugaro
Affiliation:
Centre for Stellar and Planetary Astrophysics, Monash University, Clayton 3800, Victoria, Australia email: Maria.Lugaro@sci.monash.edu.au
Simon W. Campbell
Affiliation:
Astronomy and Astrophysics Group, Department Fisica i Enginyeria Nuclear, Universitat Politecnica de Catalunya, Barcelona, Spain email: simwcampbell@gmail.com
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Abstract

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Elements heavier than iron are produced in asymptotic giant branch (AGB) stars via the slow neutron capture process (s process). Recent observations of s-process-enriched Carbon Enhanced Metal-Poor (CEMP) stars have provided an unprecedented wealth of observational constraints on the operation of the s-process in low-metallicity AGB stars. We present new preliminary full network calculations of low-metallicity AGB stars, including a comparison to the composition of a few s-process rich CEMP stars. We also discuss the possibility of using halo planetary nebulae as further probes of low-metallicity AGB nucleosynthesis.

Keywords

stars: abundances – stars: AGB and post-AGB
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Symposium S265: Chemical Abundances in the Universe: Connecting First Stars to Planets , August 2009 , pp. 57 - 60
Copyright
Copyright © International Astronomical Union 2010

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