Evolutionary timescales from the AGB to the CSPNe phase
  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.
