Abstract
ABSTRACTWe present time‐resolved CCD photometry of the recently discovered (V≃15 at maximum light) eruptive variable star in Taurus, which we dub VS 0329+1250. A total of ∼20 hr of data obtained over six nights reveal 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 minutes), which represents the shortest known superhump period 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 P˙sh≃(2.1 ± 0.8) × 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 VS 0329+1250 lies at a distance of ∼ 1.2 ± 0.2 kpc.
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