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 Porb. 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 shortperiod dwarf novae, suggesting a secondary enriched by H-burning prior to the common-envelope phase of evolution. We estimate i = 50° ± 5°, M1 = 0.63-0.09+0.12 M⊙, M2 = 0.12-0.02-0.03 M⊙, R2 = 0.121-0.007-0.010 R., and a distance to the binary of 180 ± 40 pc.
|Original language||English (US)|
|Number of pages||6|
|Journal||Publications of the Astronomical Society of the Pacific|
|State||Published - 2002|
ASJC Scopus subject areas
- Astronomy and Astrophysics
- Space and Planetary Science