PM J03338+3320: Long-Period Superhumps in Growing Phase Following a Separate Precursor Outburst
arXiv:1604.01103 · doi:10.1093/pasj/psw046
Abstract
We observed the first-ever recorded outburst of PM J03338+3320, the cataclysmic variable selected by proper-motion survey. The outburst was composed of a precursor and the main superoutburst. The precursor outburst occurred at least 5 d before the maximum of the main superoutburst. Despite this separation, long-period superhumps were continuously seen between the precursor and main superoutburst. The period of these superhumps is longer than the orbital period by 6.0(1)% and can be interpreted to reflect the dynamical precession rate at the 3:1 resonance for a mass ratio of 0.172(4). These superhumps smoothly evolved into those in the main superoutburst. These observations provide the clearest evidence that the 3:1 resonance is triggered by the precursor outburst, even if it is well separated, and the resonance eventually causes the main superoutburst as predicted by the thermal-tidal instability model. The presence of superhumps well before the superoutburst cannot be explained by alternative models (the enhanced mass-transfer model and the pure thermal instability model) and the present observations give a clear support to the thermal-tidal instability model.
arXiv comment11 pages, 4 figures, accepted for publication in PASJ (includes supporting information)
References in corpus (16)
- First Results from the Catalina Real-time Transient Survey
- Kepler Mission Design, Realized Photometric Performance, and Early Science
- Survey of Period Variations of Superhumps in SU UMa-Type Dwarf Novae
- Variable Star Network: World Center for Transient Object Astronomy and Variable Stars
- WZ Sge-Type Dwarf Novae
- Survey of Period Variations of Superhumps in SU UMa-Type Dwarf Novae. II: The Second Year (2009-2010)
- Is evidence for enhanced mass transfer during dwarf-nova outbursts well substantiated?
- New Method to Estimate Binary Mass Ratios by Using Superhumps
- The Cause of the Superoutburst in SU UMa Stars is Finally Revealed by Kepler Light Curve of V1504 Cygni
- Study of Superoutbursts and Superhumps in SU UMa Stars by the Kepler Light Curves of V344 Lyrae and V1504 Cygni
- The Kepler light curves of V1504 Cygni and V344 Lyrae: A study of the Outburst Properties
- The Kepler Light Curve of V344 Lyrae: Constraining the Thermal-Viscous Limit Cycle Instability
- Survey of Period Variations of Superhumps in SU UMa-Type Dwarf Novae. VI: The Sixth Year (2013-2014)
- A Further Study of Superoutbursts and Superhumps in SU UMa Stars by the Kepler Light Curves of V1504 Cygni and V344 Lyrae
- V1006 Cygni: Dwarf Nova Showing Three Types of Outbursts and Simulating Some Features of the WZ Sge-Type Behavior
- Cataclysmic Variables in the SUPERBLINK Proper Motion Survey