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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ASASSN-14ho：具有多次再亮化的最长周期矮新星

矮新星和X射线新星爆发后的再亮现象仍然是吸积盘理论最具挑战性的课题之一。人们普遍认为，爆发后的再亮是 WZ Sge 型矮新星的一个关键特征，其主要具有短（$\lesssim$0.06 d）轨道周期。我在 2014 年爆发期间在 ASASSN-14ho 中发现了四次爆发后的再亮化，最近测量其轨道周期异常长 [0.24315(10) d]。使用文献中径向速度研究的正式解决方案，我讨论了该物体可能是 3:1 共振稳定边界附近的 SU UMa 型矮新星的可能性，尽管它的轨道周期非常长。