ASASSN-14ho: Longest-period Dwarf Nova with Multiple Rebrightenings

Abstract

The post-outburst rebrightening phenomenon in dwarf novae and X-ray novae is still one of the most challenging subjects for theories of accretion disks. It has been widely recognized that post-outburst rebrightenings are a key feature of WZ Sge-type dwarf novae, which predominantly have short ($\lesssim$0.06 d) orbital periods. I found four post-outburst rebrightenings in ASASSN-14ho during its 2014 outburst, whose orbital period has recently measured to be exceptionally long [0.24315(10) d]. Using the formal solution of the radial velocity study in the literature, I discuss the possibility that this object can be an SU UMa-type dwarf nova near the stability border of the 3:1 resonance despite its exceptionally long orbital period. Such objects are considered to be produced if mass transfer occurs after the secondary has undergone significant nuclear evolution and they may be hidden in a significant number among dwarf novae showing multiple post-outburst rebrightenings.

4 pages, 1 figure, accepted for publication in PASJ

References in corpus (7)

• The All-Sky Automated Survey for Supernovae (ASAS-SN) Light Curve Server v1.0
• The Donor Stars of Cataclysmic Variables
• Population Synthesis of Cataclysmic Variables: I. Inclusion of Detailed Nuclear Evolution
• Comprehensive simulations of superhumps
• SU Uma stars: Rebrightenings after superoutburst
• ASAS-SN 13cl : A Newly-Discovered Cataclysmic Binary with an Anomalously Warm Secondary
• Suzaku Observations of Spectral Variations of the Ultra Luminous X-ray Source Holmberg IX X-1

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• New Candidates for AM Canum Venaticorum Stars among ASAS-SN Transients