Waves in an accretion disk: nodal superhumps versus permanent superhumps in V378 Pegasi

First science results from a new observatory, Fresno State's station at Sierra Remote Observatories, are presented.~ The nova-like cataclysmic variable V378 Pegasi (PG 2337+300) is discovered to show variable, often sawtooth-wave variations in its light curve, which have a period of 3.22 hours.~ These variations are present in light curves taken in 2001, 2008, and 2009, and have amplitudes between 0.2 and 0.4 magnitudes, as detected through a clear filter.~ We identify these as waves in this close binary star system's accretion disk, which are related to the superhump phenomenon shown by SU UMa stars.~ We also present the results of a radial velocity study to measure the orbital period, and discuss physical models for the variation in V378 Peg: either permanent superhumps, in which the disk is made elliptical and precessed by tidal forces from the stars' pronounced mass ratio, or nodal superhumps, from a tilted disk.~ We also discuss the evolutionary status of V378 Peg: at just above the period gap, this system may provide a critical test of cataclysmic variable evolution theory.