  In the light of the recent and unexpected discovery of a brand new type of
white dwarfs, those with carbon-dominated atmospheres, we examine the
asteroseismological potential of such stars. The motivation behind this is
based on the observation that past models of carbon-atmosphere white dwarfs
have partially ionized outer layers that bear strong resemblance with those
responsible for mode excitation in models of pulsating DB (helium-atmosphere)
and pulsating DA (hydrogen-atmosphere) white dwarfs. Our exciting main result
is that, given the right location in parameter space, some carbon-atmosphere
white dwarfs are predicted to show pulsational instability against gravity
modes. We are eagerly waiting the results of observational searches for
luminosity variations in these stars.
