SIMBAD references

We report photometry of a recently discovered dwarf nova with a remarkably short 64.2 minute orbital period. In quiescence, the star's light curve is that of a double sinusoid, arising from the ``ellipsoidal'' distortion of the Roche-lobe-filling secondary. During superoutburst, common superhumps develop with a period 3%-4% longer than P_orb. This indicates a mass ratio M₂/M₁=0.19±0.02, a surprisingly large value in so compact a binary. This implies that the secondary star has a density 2-3 times higher than that of other short-period dwarf novae, suggesting a secondary enriched by H-burning prior to the common-envelope phase of evolution. We estimate i=50°±5°, M₁=0.63^+0.12_–0.09 M_☉, M₂=0.12^+0.03_–0.02 M_☉, R₂=0.121^+0.010_–0.007 R_☉, and a distance to the binary of 180±40 pc.