Superhumps in Cataclysmic Binaries. V. V503 Cygni

Details Superhumps in Cataclysmic Binaries. V. V503 Cygni Superhumps in Cataclysmic Binaries. V. V503 Cygni

Jun 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995pasp..107..551h&link_type=abstract

Publications of the Astronomical Society of the Pacific, v.107, p.551

Astronomy and Astrophysics

Astronomy

72

Cataclysmic Variables, Binaries: Close

Scientific paper

We report a radial-velocity study of the dwarf nova V503 Cygni at quiescence, revealing motion of the emission lines with a period of 111.9 +- 0.4 min. This is almost certainly the underlying orbital period of the binary. We also report photometry at all stages of the outburst cycle, which demonstrates a complex pattern of signals. In superoutburst, the star shows a periodic signal at 116.7 +- 0.1 min, which bears all the earmarks of a "superhump," a normal trait of SU UMa-type dwarf nova. During quiescence and short eruptions, the star shows a large-amplitude wave at a period of 109.00 +- 0.02 min--a "negative superhump" since the period shift from P_orb is negative. We interpret the two superhumps as respectively arising from apsidal and nodal precession of the accretion disk. (SECTION: Stars)

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