  We calculate and explore an extensive adiabatic model grid for pulsating
white dwarfs with H dominated atmospheres, the ZZ Ceti stars. We also compared
the computed modes with the observed ones for five ZZ Ceti stars that are a
representative sample of the whole class of pulsators. We describe our new
approach for seismological studies, using the relative observed amplitudes to
give weights for the periods in the fit and the external mass and temperature
determinations as a guide. Our seismological study is clear evidence that
seismology is indeed a powerful tool in the study of stellar structure and
evolution.
