Abstract
Compact structure in the 1665 MHz OH emission from the long-period variable star U Orionis was detected using a five-telescope VLBI array. The U Orionis spectrum contains many compact, highly circularly polarized features which are spread over an area about 0''.5 in size. The polarization of the 1665 MHz emission from U Orionis cannot be understood by a simple Zeeman model. The extent of the main-line emission from U Orionis is significantly larger than that of previously measured 1612 MHz emission. This result is at odds with current models of circumstellar maser emission which predict that the main-line masers should lie closer to the central star than do the 1612 MHz masers.
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