Detection of Change in Supercycles in ER Ursae Majoris
arXiv:1212.5940 · doi:10.1093/pasj/65.3.54
Abstract
We examined data on about 20 years of observations of ER UMa available in AAVSO, VSNET, AFOEV, NSVS, VSOLJ databases together with published light curves. The obtained O-C diagram revealed a systematic change of the supercycle (time interval between two successive superotbursts) within 43.6 and 59.2 d. The time-scale of this change variation is from 300 to 1900 d. The number of normal outbursts within the supercycles also varied from 4 to 6 although no strong correlation between this number and supercycle length was found. We suggest that appearance of negative superhumps is responsible for the observed variations of number of normal outbursts. Our results generally confirms the expectations by the thermal-tidal instability theory.
10 pages, 6 figures, accepted for publication in PASJ
References in corpus (4)
Cited by in corpus (9)
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- Survey of Period Variations of Superhumps in SU UMa-Type Dwarf Novae. VII: The Seventh Year (2014-2015)
- Survey of Period Variations of Superhumps in SU UMa-Type Dwarf Novae. VI: The Sixth Year (2013-2014)
- Analysis of Three SU UMa-Type Dwarf Novae in the Kepler Field
- Study of Negative and Positive Superhumps in ER Ursae Majoris
- Survey of Period Variations of Superhumps in SU UMa-Type Dwarf Novae. X: The Tenth Year (2017)
- RZ Leonis Minoris Bridging between ER Ursae Majoris-Type Dwarf Nova and Novalike System
- Detection of the Supercycle in V4140 Sagittarii: First Eclipsing ER Ursae Majoris-like Object