Tidal Instability and Superhump by a Wave-Wave Resonant Model

Abstract

On a disk deformed to a non-axisymmetric form, a set of oscillations can be excited by their resonant interaction through the disk deformation (Kato et al. 2011). This resonant instability process has been proposed to suggest a possible cause of the high-frequency quasi-periodic oscillations (HF QPOs) observed in black-hole low-mass X-ray binaries. In the present paper, we examine whether the above-mentioned wave-wave resonant process can describe the tidal instability and superhump in dwarf novae. The results show that the process seems to well describe the observations. If this process is really the cause of the tidal instability and superhump, a two-armed oscillation with high frequency roughly on the magnitude of three times the orbital frequency is present on disks, although its expected amplitude may be small.

16 pages, 6 figures, accepted in PASJ

References in corpus (3)

• X-ray Properties of Black-Hole Binaries
• The dynamics of eccentric accretion discs in superhump systems
• Mean-motion resonances in satellite-disc interactions

Cited by in corpus (5)

• The Cause of the Superoutburst in SU UMa Stars is Finally Revealed by Kepler Light Curve of V1504 Cygni
• Resonant Excitation of Disk Oscillations in Deformed Disks VI: Stability Criterion Revisited
• Resonant Excitation of Tilt Mode in Tidally Deformed Disks
• Resonant Excitation of Disk Oscillations in Deformed Disks VII: Stability Criterion in MHD Systems
• Simultaneous Resonant Excitation of Low-frequency Eccentric Wave and Tilt Wave on Tidally Deformed Disks