Superhumps in VY Aquarii

Details Superhumps in VY Aquarii Superhumps in VY Aquarii

Jan 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993pasp..105...69p&link_type=abstract

Astronomical Society of the Pacific, Publications (ISSN 0004-6280), vol. 105, no. 683, p. 69-77.

Astronomy and Astrophysics

Astronomy

69

Dwarf Novae, Light Curve, Stellar Models, Stellar Orbits, Stellar Oscillations, Stellar Spectrophotometry

Scientific paper

Observations of VY Aquarii obtained both in quiescence and eruption that emphasize the great similarity of the star to well-credentialed dwarf novae like WZ Sagittae are presented. Long-term visual and photographic coverage shows two types of eruptions, differing in brightness and time scale by a factor of about 5. A transient wave in the quiescent light curve suggests a period in the range 80-120 min, which could be the orbital period of the underlying binary. Photometry during a long eruption in 1986 showed a large-amplitude modulation ('superhump') with a period of 92.7 min, which slowly decreased during the eruption. The superhumps observed in SU UMa stars appear to exhibit a similar degree of period instability, such that P-dot is approximately equal to -(3-10) x 10 exp -5.

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