http://arxiv.org/abs/1910.01013
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 ($0.8 \lesssim M_{\rm ZAMS}/M_\odot\lesssim 8…10$). 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.
M. Bertolami
Thu, 3 Oct 19
59/59
Comments: 10 pages, 6 figures, includes comments and discussion at the end. Invited review at the IAU Symposium No. 343 “Why Galaxies Care About AGB stars IV” in Vienna (2018)
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