Detection of superhumps in the VY Scl-type nova-like variable KR Aur

Abstract

We report on detection of negative superhumps in KR Aur which is the representative member of the VY Scl stars. The observations were obtained with the multi-channel photometer during 107 h. The analysis of the data clearly revealed brightness variations with a period of 3.771 +/- 0.005 h. This is 3.5 per cent less than the orbital period, suggesting it is a negative superhump. Negative superhumps in VY Scl stars are widely spread. The discovery of powerful soft X-rays from V751 Cyg demonstrates that VY Scl stars may contain white dwarfs, at which nuclear burning of the accreted material occur. If this suspicion is correct, we then can suppose that the powerful radiation emerging from the white dwarf may cause the tilt of the accretion disk to the orbital plane, and its retrograde precession may produce negative superhumps in VY Scl stars.

6 pages, 6 figures, will be published in MNRAS

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Cited by in corpus (13)

• SPH Simulations of Negative (Nodal) Superhumps: A Parametric Study
• Earth, Moon, Sun, and CV Accretion Disks
• SPH simulations of irradiation-driven warped accretion discs and the long periods in X-ray binaries
• Atlas of Tilted Accretion Disks & Source to Negative Superhumps
• TESS light curves of cataclysmic variables -- II: Superhumps in old novae and novalike variables
• TT Arietis: 40 years of photometry
• When the disc's away, the stars will play: dynamical masses in the nova-like variable KR Aur with a pinch of accretion
• Tilted discs in six poorly studied cataclysmic variables
• Photometry of some more neglected bright cataclysmic variables and candidates
• Photometry of some neglected bright cataclysmic variables and candidates
• Long-term Periodicities of Cataclysmic Variables with Synoptic Surveys
• Cyclic variations with twice the accretion disk precession period in the old nova V603 Aquilae
• Accretion Discs with an Inner Spiral Density Wave