Time-resolved CCD photometry is presented of the recently-discovered ( V \simeq 15 at maximum light ) eruptive variable star in Taurus , which we dub VS0329+1250 .
A total of \sim 20 hr of data obtained over six nights reveals superhumps in the light curves , confirming the star as a member of the SU UMa class of dwarf novae .
The superhumps recur with a mean period of 0.053394 ( 7 ) days ( 76.89 min ) , which represents the shortest superhump period known in a classical SU UMa star .
A quadratic fit to the timings of superhump maxima reveals that the superhump period was increasing at a rate given by \dot { P } _ { \mathrm { sh } } \simeq ( 2.1 \pm 0.8 ) \times 10 ^ { -5 } over the course of our observations .
An empirical relation between orbital period and the absolute visual magnitude of dwarf novae at maximum light , suggests that VS0329+1250 lies at a distance of \sim 1.2 \pm 0.2 kpc .