New asymptotic giant branch models for a range of metallicities
Weiss, Achim Ferguson, Jason W.
Weiss, Achim
Ferguson, Jason W.
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2009-11-19
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Article
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Keywords
Stars: Agb And Post-agb,Stars: Evolution,Stars: Interiors,Asymptotic Giant Branch,Carbon Stars,Carbon-enriched,Chemical Mixtures,Effective Temperature,Input Datas,Low Temperatures,Mass Loss,Mass Loss Rate,Metal Ratio,Metallicities,Post-agb,Stars:agb And Post Agb,Stellar Envelope,Stellar Models,Synthetic Models,Stars: Evolution,Stars: Interiors,Asymptotic Analysis,Chemical Elements,Models,Opacity,Oxygen,Carbon,Stars
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Citation
New asymptotic giant branch models for a range of metallicities A. Weiss and J. W. Ferguson A&A, 508 3 (2009) 1343-1358 DOI: https://doi.org/10.1051/0004-6361/200912043
Abstract
We present a new grid of stellar model calculations for stars on the Asymptotic Giant Branch between 1.0 and 6.0 M. Our grid consists of 10 chemical mixtures with 5 metallicities between Z = 0.0005 and Z = 0.04, and with both solar-like and α-element enhanced metal ratios for each metallicity. We treat consistently the carbon-enhancement of the stellar envelopes by using opacity tables with varying C/O-ratio and by employing theoretical mass loss rates for carbon stars. The low temperature opacities have been calculated specifically for this project. For oxygen stars we use an empirical mass loss formalism. The third dredge-up is naturally obtained by including convective overshooting. Our models reach effective temperatures in agreement with earlier synthetic models, which included approximative carbon-enriched molecular opacities and show good agreement with empirically determined carbon-star lifetimes. A fraction of the models could be followed into the post-AGB phase, for which we provide models in a mass range supplementing previous post-AGB calculations. Our grid constitutes the most extensive set of AGB-models, calculated with the latest physical input data and treating carbon-enhancement due to the third dredge-up most consistently. © 2009 ESO. © 2010 Elsevier B.V., All rights reserved.
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This is an open access article under the CC BY license.
Publisher
EDP Sciences
Journal
Astronomy and Astrophysics
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0004-6361
1432-0746
1432-0746