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We calculate and explore an extensive adiabatic model grid for pulsating white dwarfs with hydrogen‐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.

Seismological studies of ZZ Ceti stars – I. The model grid and the application to individual stars