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Heavy Element Abundances in Planetary Nebulae: A Theorist's Perspective

Published online by Cambridge University Press:  02 January 2013

Amanda I. Karakas  and
Maria Lugaro
Amanda I. Karakas*
Affiliation:
Research School of Astronomy & Astrophysics, Mount Stromlo Observatory, Cotter Road Weston Creek, ACT 2611
Maria Lugaro
Affiliation:
Centre for Stellar and Planetary Astrophysics, Monash University, PO Box 28M, Clayton, Vic 3800
*
CCorresponding author. Email: [email protected]
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Abstract

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The determination of heavy element abundances from planetary nebula (PN) spectra provides an exciting opportunity to study the nucleosynthesis occurring in the progenitor asymptotic giant branch (AGB) star. We perform post-processing calculations on AGB models of a large range of mass and metallicity to obtain predictions for the production of neutron-capture elements up to the first s-process peak at strontium. We find that solar metallicity intermediate-mass AGB models provide a reasonable match to the heavy element composition of Type I PNe. Likewise, many of the Se and Kr enriched PNe are well fitted by lower mass models with solar or close-to-solar metallicities. However, those objects most enriched in Krand those PN with sub-solar Se/O ratios are difficult to explain with AGB-nucleosynthesis models. Furthermore, we compute s-process abundance predictions for low-mass AGB models of very low metallicity ([Fe/H]≈−2.3) using both scaled solar and an α-enhanced initial composition. For these models, O is dredged to the surface, which means that abundance ratios measured relative to this element (e.g. X/O) do not provide a reliable measure of initial abundance ratios, or of production within the star owing to internal nucleosynthesis.

Keywords

abundancesISM: abundancesplanetary nebulae: generalstars: AGB and post-AGB
Type
Research Article
Information
Publications of the Astronomical Society of Australia , Volume 27 , Issue 2 , 2010 , pp. 227 - 231
Copyright
Copyright © Astronomical Society of Australia 2010

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