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AGB Stars and the Observed Abundance of Neon in Planetary Nebulae

Published online by Cambridge University Press:  05 March 2013

A. I. Karakas  and
J. C. Lattanzio
A. I. Karakas
Affiliation:
Centre for Stellar and Planetary Astrophysics, School of Mathematical Sciences, Monash University, Melbourne 3800, Australia Institute for Computational Astrophysics, Department of Astronomy & Physics, Saint Mary’s University, Halifax, Canada; akarakas@ap.stmarys.ca
J. C. Lattanzio
Affiliation:
Centre for Stellar and Planetary Astrophysics, School of Mathematical Sciences, Monash University, Melbourne 3800, Australia; john.lattanzio@sci.monash.edu.au.
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Abstract

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Asymptotic giant branch stars are expected to produce 22Ne through the combined H and He burning that operates during their thermally pulsing evolution. However, observationally there is a fairly tight correlation between the O and Ne abundances as measured in planetary nebulae in various populations. In this paper we use recent detailed stellar evolutionary calculations for compositions appropriate to the Galaxy and the Large Magellanic Cloud, in an attempt to determine if the models are consistent with the observed abundances. We show that there is only a narrow range in stellar mass, about 2 to 4 M⊙ (lower for lower [Fe/H]) where 22Ne is produced in sufficient quantities to affect the total observed elemental neon abundance, which is mostly 20Ne. The models appear to be consistent with the observations, but a more thorough analysis is required.

Keywords

stars: AGB and post-AGBstars: abundancesstars: interiorsstars: low massISM: abundancesplanetary nebulae: generalneon
Type
Sixth Torino Workshop
Information
Publications of the Astronomical Society of Australia , Volume 20 , Issue 4 , 2003 , pp. 393 - 400
Copyright
Copyright © Astronomical Society of Australia 2003

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