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Evolutionary timescales from the AGB to the CSPNe phase

Published online by Cambridge University Press:  30 December 2019

Marcelo M. Miller Bertolami Open the ORCID record for Marcelo M. Miller Bertolami [Opens in a new window]
Marcelo M. Miller Bertolami*
Affiliation:
Instituto de Astrofísica de La Plata, CCT-La Plata, CONICET-UNLP, Paseo del Bosque s/n (B1900FWA), La Plata, Argentina email: mmiller@fcaglp.unlp.edu.ar Universidad Nacional de La Plata Paseo del Bosque s/n (B1900FWA), La Plata, Argentina
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Abstract

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The transition from the asymptotic giant branch (AGB) to the final white dwarf (WD) stage is arguably the least understood phase in the evolution of single low- and intermediate-mass stars (0.8 ≲ MZAMS/M⊙ ≲ 8…10). Here we briefly review the progress in the last 50 years of the modeling of stars during the post-AGB phase. We show that although the main features, like the extreme mass dependency of post-AGB timescales were already present in the earliest post-AGB models, the quantitative values of the computed post-AGB timescales changed every time new physics was included in the modeling of post-AGB stars and their progenitors. Then we discuss the predictions and uncertainties of the latest available models regarding the evolutionary timescales of post-AGB stars.

Keywords

stars: AGB and post-AGBplanetary nebulae: generalstars: evolutionstars: mass loss
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 14 , Symposium S343: Why Galaxies Care About AGB Stars: A Continuing Challenge through Cosmic Time , August 2018 , pp. 36 - 46
Copyright
© International Astronomical Union 2019 

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