  We study the formation and evolution of DA white dwarfs, the progenitors of
which have experienced a late thermal pulse (LTP) shortly after the departure
from the thermally pulsing AGB. To this end, we compute the complete evolution
of an initially 2.7 Mo star all the way from the zero-age main sequence to the
white dwarf stage. We find that most of the original H-rich material of the
post-AGB remnant is burnt during the post-LTP evolution, with the result that,
at entering its white dwarf cooling track, the remaining H envelope becomes
10^-6 Mo in agreement with asteroseismological inferences for some ZZ Ceti
stars.
