We have derived the luminosity function for stars in the bulge of M31 in a region ∼7.2′ (1.44 kpc) from its nucleus. It has an upper limit ∼0.5 mag brighter than the steep cutoff observed in the Galactic bulge luminosity function. The shape of our M31 luminosity function, that of Rich and Mould for a region 4.1′ from the nucleus, and the differences between them are all consistent with a model based on a Galactic bulge luminosity function modified by the addition of disk stars located behind M31's bulge. Kent's disk/bulge deconvolution of M31 is used to fix independently the relative amounts of disk contamination at different radii. There is no compelling reason to invoke a stellar population for the bulge of M31 that differs from that of the bulge of our own Galaxy