On supercycle lengths of active SU UMa stars
arXiv:1303.6248 · doi:10.1093/mnras/stt815
Abstract
We performed a detailed analysis of extensive photometric observations of a sample of most active dwarf novae, that is SU UMa stars which are characterised by supercycle lengths shorter than 120 days. We found the observational evidence that supercycle lengths for these objects have been constantly increasing over the past decades, which indicates that their mean mass transfer rates have been decreasing during that time. This seems to be a common feature for this type of stars. We present numerical results in each case and estimate time scales of future development of these systems. This study is important in the context of evolution of dwarf novae stars and perhaps other cataclysmic variables.
7 pages, 6 figures, submitted to MNRAS
References in corpus (5)
- Achieving better than 1 minute accuracy in the Heliocentric and Barycentric Julian Dates
- The Shape of Long Outbursts in U Gem Type Dwarf Novae from AAVSO Data
- IX Draconis - a curious ER UMa-type dwarf nova
- Curious Variables Experiment (CURVE). CCD photometry of active dwarf nova DI UMa
- Curious Variables Experiment (CURVE). Variable properties of the dwarf nova SS UMi
Cited by in corpus (6)
- Statistical analysis of properties of dwarf novae outbursts
- Cataclysmic Variables observed during K2 Campaigns 0 and 1
- RZ Leonis Minoris Bridging between ER Ursae Majoris-Type Dwarf Nova and Novalike System
- MN Draconis - peculiar, active dwarf nova in the period gap
- Transient behavior of three SU UMa-type dwarf novae; AR Pic, QW Ser and V521 Peg
- Detection of the Supercycle in V4140 Sagittarii: First Eclipsing ER Ursae Majoris-like Object