2019/09/03 by Taichi Kato, Franz-Josef Hambsch, Berto Monard +3
Physics and Astronomy · #Accretion (finance) #Accretion disc #Astronomy and Astrophysical Research #Astrophysical Phenomena and Observations #Cataclysmic variable star #Dwarf nova #Gamma-ray bursts and supernovae #Instability #Low Mass #White dwarf #astro-ph.SR
paper · pdf · doi:10.1093/pasj/psz108
5 pages, 4 figures, accepted for publication in PASJ
arxiv created 2019/09/03 · openalex publication_date 2019/09/04 · openalex created_date 2019/09/12 · arxiv updated 2020/01/08 · openalex updated_date 2026/08/05
Abstract We observed the 2018 November outburst of CS Ind and confirmed that it was a genuine superoutburst with a very long [0.12471(1) d on average] superhump period. The superoutburst was preceded by a long precursor, which was recorded for the first time in SU UMa-type dwarf novae. Our interpretation is that the combination of a sufficient amount of mass in the disk before the ignition of the outburst and the slow development of tidal instability near the borderline of the 3 : 1 resonance caused a cooling front to start before the full development of tidal instability. This finding provides more support to the recent interpretation of slow development of the tidal instability causing various phenomena similar to WZ Sge-type dwarf novae in SU UMa-type dwarf novae with very long orbital periods.