Detection of the Supercycle in V4140 Sagittarii: First Eclipsing ER Ursae Majoris-like Object
arXiv:1804.02107 · doi:10.1093/pasj/psy049
Abstract
We observed the deeply eclipsing SU UMa-type dwarf nova V4140 Sgr and established the very short supercycle of 69.7(3) d. There were several short outbursts between superoutbursts. These values, together with the short orbital period (0.06143 d), were similar to, but not as extreme as, those of ER UMa-type dwarf novae. The object is thus the first, long sought, eclipsing ER UMa-like object. This ER UMa-like nature can naturally explain the high (apparent) quiescent viscosity and unusual temperature profile in quiescence, which were claimed observational features against the thermal-tidal instability model. The apparently unusual outburst behavior can be reasonably explained by a combination of this ER UMa-like nature and the high orbital inclination and there is no need for introducing mass transfer bursts from its donor star.
5 pages, 1 figure, accepted for publication in PASJ
References in corpus (5)
- An accurate geometric distance to the compact binary SS Cygni vindicates accretion disc theory
- A Further Study of Superoutbursts and Superhumps in SU UMa Stars by the Kepler Light Curves of V1504 Cygni and V344 Lyrae
- Survey of Period Variations of Superhumps in SU UMa-Type Dwarf Novae. IX: The Ninth Year (2016-2017)
- Study of Negative and Positive Superhumps in ER Ursae Majoris
- SOAR observations of the high-viscosity accretion disc of the dwarf nova V4140 Sagitarii in quiescence and in outburst