  ZZ Ceti stars are pulsating white dwarfs with a carbon-oxygen core (or
possibly ONe for the most massive stars) build up during the core helium
burning (CHeB) and thermally pulsing Asymptotic Giant Branch (TP-AGB) phases.
Through the interpretation of their pulsation periods by means of
asteroseismology, details about their origin and evolution can be inferred. The
whole pulsation spectrum exhibited by ZZ Ceti stars strongly depend on the
inner chemical structure. At present, there are several processes affecting the
chemical profiles that are still not accurately determined. We present a study
of the impact of current uncertainties in the evolution of white dwarf
progenitor on the expected pulsation properties and on the stellar parameters
inferred from asteroseismological fits of ZZ Ceti stars. Our analysis is based
on a set of carbon-oxygen core white dwarf models that are derived from full
evolutionary computations from the ZAMS to the ZZ Ceti domain. We considered
models in which we varied the number of thermal pulses, the amount of
overshooting, and the carbon-alpha reaction rate within their uncertainties. We
explore the impact of these major uncertainties in prior evolution on the
chemical structure and expected pulsation spectrum. We find that these
uncertainties yield significant changes in the g-mode pulsation periods being
those found during the TP-AGB phase the most relevant for the pulsational
properties and the asteroseismological derived stellar parameters of ZZ Ceti
stars. We conclude that the uncertainties in the white dwarf progenitor
evolution should be taken into account in detailed asteroseismological analyses
of these pulsating stars.
