Context : 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The two grids of models presently available are based on outdated micro- and macrophysics and do not agree with each other .
Studies of the central stars of planetary nebulae ( CSPNe ) and post-AGB stars in different stellar populations point to significant discrepancies with the theoretical predictions of post-AGB models .

Aims : We study the timescales of post-AGB and CSPNe in the context of our present understanding of the micro- and macrophysics of stars .
We want to assess whether new post-AGB models , based on the latter improvements in TP-AGB modeling , can help us to understand the discrepancies between observation and theory and within theory itself .
In addition , we aim to understand the impact of the previous AGB evolution for post-AGB phases .

Methods : We computed a grid of post-AGB full evolutionary sequences that include all previous evolutionary stages from the zero age main sequence to the white dwarf phase .
We computed models for initial masses between 0.8 and 4 M _ { \odot } and for a wide range of initial metallicities ( Z _ { 0 } = 0.02 , 0.01 , 0.001 , 0.0001 ) .
This allowed us to provide post-AGB timescales and properties for H-burning post-AGB objects with masses in the relevant range for the formation of planetary nebulae ( \sim 0.5 \mbox { - - } 0.8 M _ { \odot } ) .
We included an updated treatment of the constitutive microphysics and included an updated description of the mixing processes and winds that play a key role during the thermal pulses ( TP ) on the AGB phase .

Results : We present a new grid of models for post-AGB stars that take into account the improvements in the modeling of AGB stars in recent decades .
These new models are particularly suited to be inputs in studies of the formation of planetary nebulae and for the determination of the properties of CSPNe from their observational parameters .
We find post-AGB timescales that are at least approximately three to ten times shorter than those of old post-AGB stellar evolution models .
This is true for the whole mass and metallicity range .
The new models are also \sim 0.1 \mbox { - - } 0.3 dex brighter than the previous models with similar remnant masses .
Post-AGB timescales only show a mild dependence on metallicity .

Conclusions : The shorter post-AGB timescales derived in the present work are in agreement with recent semiempirical determinations of the post-AGB timescales from the CSPNe in the Galactic bulge .
The lower number of post-AGB and CSPNe predicted by the new models might help to alleviate some of the discrepancies found in the literature .
As a result of the very different post-AGB crossing times , initial final mass relation and luminosities of the present models , the new models will have a significant impact on the predictions for the formation of planetary nebulae and the planetary nebulae luminosity function .
In particular , the new models should help to understand the formation of low-mass CSPNe as inferred from asteroseismic and spectroscopic determinations .