The need for independent methods to determine the global parameters of white dwarf stars motivates the development of a new “seismic technique” for characterizing pulsating white dwarfs. This technique combines precision measurements of white dwarf pulsation periods with Gaia parallaxes in a probability estimate of mass and effective temperature (Teff). The measured quantities of mean pulsation period spacing and absolute G-band magnitude each permit solutions that follow monotonic trends in the mass–Teff. plane, but in opposing directions. The work of this poster focuses on the determination of the mean period spacing of 10 helium atmosphere white dwarf stars.?