The 2000-2001 Superoutburst of the WZ Sge-Type Star RZ Leonis : A Clue to Understanding the Origin of Viscosity in Quiescent Dwarf Nova Disks
The 2000-2001 Superoutburst of the WZ Sge-Type Star RZ Leonis : A Clue to Understanding the Origin of Viscosity in Quiescent Dwarf Nova Disks
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2000-2001 年 WZ Sge 型恒星 RZ Leonis 的超级爆发：了解静止矮新星盘粘度起源的线索
DOI：
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发表时间：
2001
期刊：
影响因子：
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通讯作者：
H. Kawakita
中科院分区：
文献类型：
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作者：
R. Ishioka;Taichi Kato;M. Uemura;H. Iwamatsu;K. Matsumoto;R. Stubbings;R. Mennickent;G. Billings;S. Kiyota;G. Masi;J. Pietz;R. Novák;B. Martin;A. Oksanen;M. Moilanen;K. Torii;K. Kinugasa;H. Kawakita
我们在此报告发生在2000年12月至2001年1月间的矮新星RZ Leo超爆发的时间分辨光度观测结果。根据我们的观测，我们揭示了突出的以下特征：持续时间长，振幅大，存在两种类型的超级峰——“早期超级峰”和“正常超级峰”。除了爆发频率极低外，爆发的特征强烈表明RZ狮子座是WZ sge型矮新星的第五成员。RZ Leo的轨道周期为0.07651 d，比其他WZ Sge恒星的“标准”周期（~ 0.058 d）要长得多。较长的周期表明RZ狮子座是非简并的次级星系，这表明由简并褐矮星次级星系引起的低静止粘度的想法可能是不正确的。目前发现的RZ Leo是WZ Sge恒星，首次清楚地表明，静止WZ Sge恒星吸积盘中磁湍流的衰减在产生所提出的低静止粘度中起着重要作用。
We report here on time-resolved photometric observations of the superoutburst of a dwarf nova, RZ Leo, which occurred during 2000 December–2001 January. We reveal the following characteristics of the outburst based on our observations: long duration, large amplitude, and the existence of two types of superhumps — “early superhumps” and “normal superhumps”. In addition to the extremely low frequency of the outbursts, the characteristics of the outburst strongly indicate that RZ Leo is the fifth member of the WZ Sge-type dwarf novae. The orbital period of RZ Leo is 0.07651 d, which is remarkably longer than the “canonical” period of other WZ Sge stars (∼ 0.058 d). The longer period indicates a non-degenerate secondary of RZ Leo, which suggests that the idea of a low quiescence viscosity due to a degenerate brown dwarf secondary may not be correct. The present discovery of RZ Leo as being a WZ Sge star provides the first clear indication that the decay of magnetic turbulence in accretion disks of quiescent WZ Sge stars plays an important role in producing the proposed low quiescent viscosity.