Optical photometry of the double-lined cataclysmic variable Phoenix 1

We have obtained 7 nights of time-resolved VI photometry of the double-line d cataclysmic variable Phoenix 1. We detect two candidate orbital periods, 0.1344 day and 0.2683 day. The former, which would correspond to a single m odulation caused by viewing the irradiated face of the secondary star, is t he less favored choice based on the folded light curves. The latter, which would correspond to a double modulation with unequal minima depths caused b y ellipsoidal variation of the secondary star, is inconsistent with the obs erved late spectral type (M2-5) of the secondary star. However, we discuss some recent results from the literature that may make it possible to reconc ile the longer orbital period and later spectral type. Some ambiguity remai ns as to which of these two periods is the true orbital period.