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 M 2 /M 1 = 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°, M 1 = 0.63 +0.12 -0.09 M ⊙ , M 2 = 0.12 +0.03 -0.02 M ⊙ , R 2 = 0.121 +0.010 -0.007 R ⊙ , and a distance to the binary of 180 ± 40 pc.
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Skillman et al. (2002) studied this question.
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