Following the recent mode identification by Clemens suggesting the hydrogen layer mass of the DAV (ZZ Ceti) stars is nearly the same, I make the extreme assumption that models with a single composition profile with a hydrogen layer mass of 1.5 × 10−4M* may be able to fit the observed pulsation periods. Because I use only a single composition profile, this seismological analysis of eight DAV stars is preliminary, pending model fits for a range of hydrogen layer masses. These models duplicate the observed periods of several hot DAV pulsators quite well, when I allow for a small spread in total mass and effective temperature. My results confirm the dominant pulsation mode power in the DAV stars resides in l = 1 modes, although a few l ≥ 2 modes are present. Assuming this hydrogen layer mass is typical for all DA white dwarfs, current theories for the evolution of stars from the asymptotic giant branch through the planetary nebula stage are at least qualitatively correct and will affect the ages and average mass of the DA white dwarfs.