Constraints on the physics of dredge-up in low mass AGB stars

Details Constraints on the physics of dredge-up in low mass AGB stars Constraints on the physics of dredge-up in low mass AGB stars

Aug 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006iaujd..11e..18b&link_type=abstract

Pre-Solar Grains as Astrophysical Tools, 26th meeting of the IAU, Joint Discussion 11, 21 August 2006, Prague, Czech Republic, J

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It is known from detailed evolution models that some thermally pulsating asymptotic giant branch (TP-AGB) stars, experience dredge-up episodes after under-going a thermal pulse, in which the (newly synthesized) material from the inter-shell is mixed into the convective envelope. However, between the results of the different detailed evolution codes there is no clear agreement on which stellar (core) masses are needed for the dredge-up to take place, and if it does, in which amount it happens. We study the abundance ratios of C, O and slow neutron capture elements in the evolutionary ending points of TP-AGB stars by carrying out stellar population synthesis, using a rapid synthetic stellar evolution code which includes an up-to-date treatment of AGB nucleosynthesis and evolution. When comparing our results to observational data of post-AGB stars we can adjust the unknown parameters in order to reproduce statistically the observations. We conclude that the dredge-up occurs in stars which have a lower mass than what is predicted by the detailed evolution models, and that when it happens, a significant amount of material is mixed into the envelope. This is the first time that this technique is used for comparing the theoretical models and the real observations. Our results are consistent with other studies which pursued constraints in the dredge-up by attempting to reproduce the luminosity function of carbon stars of the Magellanic Clouds.

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