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Abundances of Iron-Group Elements in Planetary Nebulae and Consequences for Chemical Enrichment

Published online by Cambridge University Press:  08 August 2017

Harriet L. Dinerstein Open the ORCID record for Harriet L. Dinerstein [Opens in a new window] ,
T. R. Geballe  and
N. C. Sterling Open the ORCID record for N. C. Sterling [Opens in a new window]
Harriet L. Dinerstein
Affiliation:
Department of Astronomy, University of Texas at Austin, 2515 Speedway, Stop C1400, Austin, TX 78712-1205, U.S.A. email: harriet@astro.as.utexas.edu
T. R. Geballe
Affiliation:
Gemini Observatory, 670 N Aohoku Place, Hilo, HI 96720-2700, U.S.A. email: tgeballe@gemini.edu
N. C. Sterling
Affiliation:
Deptartment of Physics, University of West Georgia, 105 Boyd Building 1601 Maple Street, Carrollton, GA 30118-0001, U.S.A. email: nsterlin@westga.edu
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Abstract

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We have developed a method for determining elemental Fe-group abundances in planetary nebulae using an infrared emission line of Zn, the least refractory Fe-group species. Many planetary nebulae, particularly those of the Milky Way’s thick disk and bulge, display subsolar [Fe/H] (as inferred from Zn) although their abundances of α elements such as O, S, and Ar are nearly solar. We discuss the implications for determining enhancements of species synthesized by the progenitor star during the AGB (e.g., s-process products), and for galactic chemical evolution in view of the metallicity dependence of AGB nucleosynthetic yields.

Keywords

planetary nebulae: generalstars: AGB and post-AGBnuclear reactionsnucleosynthesisabundances
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 12 , Symposium S323: Planetary Nebulae: Multi-Wavelength Probes of Stellar and Galactic Evolution , October 2016 , pp. 82 - 85
Copyright
Copyright © International Astronomical Union 2017 

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