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We present UBVRI photometry of N Mus 1991 (=GU Mus) over the first year following outburst. GU Mus belongs to the family of X-ray novae where the primary is believed to be a black hole, and the secondary a normal late-type dwarf. These systems exhibit secondary maxima in their X-ray light curves. We compare the temporal evolution of the optical and X-ray emission of GU Mus to those of GRO J0422+32 and V616 Mon. We find that all three sytems displayed similar optical and X-ray behavior, but on slightly different time scales. We present models for the optical spectral energy distributions of both GRO J0422+32 and GU Mus.
