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 ^ { o } .
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 \la 190 MG ) and its magnetic longitude ( \psi _ { S } \sim 330 ^ { o } ) .