New models for the evolution of central stars of planetary nebulae:
  Faster and Brighter
  The post-asymptotic giant branch (AGB) phase is arguably one of the least
understood phases of the evolution of low- and intermediate- mass stars. The
recent post-AGB evolutionary sequences computed by Miller Bertolami (2016) are
at least three to ten times faster than those previously published by
Vassiliadis & Wood (1994) and Bloecker (1995) which have been used in a large
number of studies. This is true for the whole mass and metallicity range. The
new models are also $\sim$0.1-0.3 dex brighter than the previous models with
similar remnant masses. In this short article we comment on the main reasons
behind these differences, and discuss possible implications for other studies
of post-AGB stars or planetary nebulae.
