ASASSN-14ho: Longest-period Dwarf Nova with Multiple Rebrightenings. (arXiv:1911.08093v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Kato_T/0/1/0/all/0/1">Taichi Kato</a> (Kyoto U)
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$0.06 d)
orbital periods. I found four post-outburst rebrightenings in ASASSN-14ho
during its 2014 outburst, whose orbital period has recently measured to be
exceptionally long [0.24315(10) d]. Using the formal solution of the radial
velocity study in the literature, I discuss the possibility that this object
can be an SU UMa-type dwarf nova near the stability border of the 3:1 resonance
despite its exceptionally long orbital period. Such objects are considered to
be produced if mass transfer occurs after the secondary has undergone
significant nuclear evolution and they may be hidden in a significant number
among dwarf novae showing multiple post-outburst rebrightenings.
The post-outburst rebrightening phenomenon in dwarf novae and X-ray novae is
still one of the most challenging subjects for theories of accretion disks. It
has been widely recognized that post-outburst rebrightenings are a key feature
of WZ Sge-type dwarf novae, which predominantly have short ($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.
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