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Using our new photometric and spectroscopic observations as well as allavailable published data, we present a new interpretation of the properties ofthe peculiar emission-line binary UX Mon. We conclude that this binary is in arare phase of fast mass transfer between the binary components prior to themass ratio reversal. We firmly establish that the orbital period is secularlydecreasing at a rate of $\dot{P}=-0.260$ seconds per year. From several linesof reasoning, we show that the mass ratio of the component losing mass to themass-gaining component $q$ must be larger than 1 and find our most probablevalue to be $q=1.15\pm0.1$. The BINSYN suite of programs and the steepestdescent method were used to perform the final modeling. We modeled the star asa W Ser star with a thick disk around its primary. Although the remaininguncertainties in some of the basic physical elements describing the system inour model are not negligible, the model is in fair agreement with availableobservations. Only the nature of the light variations outside the primaryeclipse remains unexplained.

UX Monocerotis as a W Serpentis binary