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R. Costero, J. Echevarria (Instituto de Astronomia, UNAM), R. Michel, S. Zharikov (Instituto de Astronomia, Ensenada, UNAM)
We report spectroscopic observations of the low-inclination dwarf nova EY Cyg, spanning eleven years. The radial velocity curves for both the emission and absorption components are determined for the first time. The orbital period is found to be 0.45932448(9) days, a value much larger than previously reported. The system inclination and, hence, the mass of each stellar component are estimated within very tight limits. In particular, we conclude that the mass of the white dwarf must be near the Chandrasekhar limit.
We also performed photometric observations, some of them simultaneous to the spectroscopic runs. The light curve shows oscillations with a period of 0.494027 days. Its deference with the orbital period is statistically significant and similar to the so-called "permanent superhumps" observed in shorter period dwarf novae. The significance of this phenomenon is analyzed.
The author(s) of this abstract have provided an email address for comments about the abstract: costero@astroscu.unam.mx
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Bulletin of the American Astronomical Society, 36 5
© 2004. The American Astronomical Society.