New Post-AGB star models as tools to understand AGB evolution and nucleosynthesis

Abstract

We study a sample of post-AGB stars in the Galaxy, with known surface chemical composition and s-process enrichment. The recent determination of the luminosities of these sources, based on Gaia parallaxes, allows for the fist time a deep investigation of Galactic post-AGB stars, with the possibility of characterising the individual objects in terms of mass, chemical composition and age of the progenitors. To this aim we used available evolutionary sequences of AGB stars, extended to the post-AGB phase, complemented by new models, specifically calculated for the present study. The combined knowledge of the surface carbon and of the luminosity proves the most valuable indicator of the previous history of the star, particularly for what regards the efficiency of the various mechanisms able to alter the surface chemical composition and the growth of the core mass. This kind of analysis allows dissecting different classes of stars, such as low-mass objects, that evolved as M-type stars for the whole AGB lifetime, carbon stars, massive AGB stars that experienced hot bottom burning. The potentialities of this approach to shed new light on still debated issues related to the AGB evolution are also commented.

arXiv commentto be submitted to MNRAS. 19 pages, 9 figures

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• A study of carbon-rich post-AGB stars in the Milky Way to understand the production of carbonaceous dust from evolved stars
• A study of oxygen-rich post-AGB stars in the Milky Way to understand the production of silicates from evolved stars
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• The role of mass loss in constraining quenching time in dwarf galaxies from AGB and RGB star counts