  We present an asteroseismic analysis of the helium atmosphere white dwarf (a
DBV) recently found in the field of view of the Kepler satellite. We analyze
the 5-mode pulsation spectrum that was produced based on one month of high
cadence Kepler data. The pulsational characteristics of the star and the
asteroseismic analysis strongly suggest that the star is hotter (29200 K) than
the 24900 K suggested by model fits to the low S/N survey spectrum of the
object. This result has profound and exciting implications for tests of the
Standard Model of particle physics. Hot DBVs are expected to lose over half of
their energy through the emission of plasmon neutrinos. Continuous monitoring
of the star with the Kepler satellite over the course of 3 to 5 years is not
only very likely to yield more modes to help constrain the asteroseismic fits,
but also allow us to obtain a rate of change of any stable mode and therefore
measure the emission of plasmon neutrinos.
