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DV UMa is an eclipsing dwarf nova with an orbital period of $\sim2.06$ h,which lies just at the bottom edge of the period gap. To detect its orbitalperiod changes we present 12 new mid-eclipse times by using our CCD photometricdata and archival data. Combining with the published mid-eclipse times inquiescence, spanning $\sim30$ yr, the latest version of the $O-C$ diagram wasobtained and analyzed. The best fit to those available eclipse timings showsthat the orbital period of DV UMa is undergoing a cyclic oscillation with aperiod of $17.58(\pm0.52)$ yr and an amplitude of $71.1(\pm6.7)$ s. Theperiodic variation most likely arises from the light-travel-time effect via thepresence of a circumbinary object because the required energy to drive theApplegate mechanism is too high in this system. The mass of the unseencompanion was derived as $M_{3}\sin{i'}=0.025(\pm0.004)M_{\odot}$. If the thirdbody is in the orbital plane (i.e. $i'=i=82.9^{\circ}$) of the eclipsing pair,it would match to a brown dwarf. This hypothetical brown dwarf is orbiting itshost star at a separation of $\sim8.6$ AU in an eccentric orbit ($e=0.44$).

Cyclic period oscillation of the eclipsing dwarf nova DV UMa