ASASSN-14ho: Longest-period dwarf nova with multiple rebrightenings
ASASSN-14ho: Longest-period dwarf nova with multiple rebrightenings
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ASASSN-14ho：具有多次再增亮的最长周期矮新星
DOI：
10.1093/pasj/psz135
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发表时间：
2019
影响因子：
2.3
通讯作者：
Taichi Kato
中科院分区：
文献类型：
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作者：
Taichi Kato
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中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，它们主要具有短（约0.06 d）的轨道周期。作者在ASASSN-14 ho的2014年爆发期间发现了四次爆发后的再亮，其轨道周期最近被测量为异常长[0.24315（10）d]。利用文献中径向速度研究的形式解，本文讨论了该天体在3：1共振稳定边界附近可能是SU UMa型矮新星的可能性，尽管它的轨道周期非常长。这些天体被认为是在次级恒星经历了重大的核演化之后发生质量转移时产生的，它们可能隐藏在大量的爆发后多次重新变亮的矮新星中。
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 (≲0.06 d) orbital periods. The author found four post-outburst rebrightenings in ASASSN-14ho during its 2014 outburst, whose orbital period was recently measured to be exceptionally long [0.24315(10) d]. Using the formal solution of the radial velocity study in the literature, this paper discusses the possibility that this object could 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 of dwarf novae showing multiple post-outburst rebrightenings.
机器人体平移-伸长循环的动力学模型
DOI：
--
发表时间：
2009
期刊：
影响因子：
--
作者：
萩原雅人;藤原理賀;鄭旭光;河江達也;松本茂紀・渡辺宙志・島田尚・伊藤伸泰
通讯作者：
松本茂紀・渡辺宙志・島田尚・伊藤伸泰