  We have obtained time-series infrared photometry for the highly magnetic
cataclysmic variable AR UMa. Our J and K' band observations occurred during a
low state and they show a distinctive double-humped structure. Using detailed
models for the expected ellipsoidal variations in the infrared due to the
non-spherical secondary star, we find that the most likely value for the system
inclination is 70 degrees. We also model low state V band photometry and find
that its observed double-humped structure is not caused by ellipsoidal
variations, as they have been ascribed to, but are due to beamed cyclotron
radiation. We use this result to estimate the magnetic field strength of the
active southern accretion region (B <= 190 MG) and its magnetic longitude (330
degrees).
