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IW And-type State in IM Eridani

Publication of the Astronomical Society of Japan(2019)

Kyoto Univ | Osaka Kyoiku Univ | Ctr Backyard Astrophys Belgium | GEOS | VSOLJ | RAS | Ctr Backyard Astrophys Pretoria | Rolling Hills Observ

Cited 10|Views23
Abstract
IW And stars are a recently recognized group of dwarf novae which are characterized by a repeated sequence of brightening from a standstill-like phase with damping oscillations followed by a deep dip. Kimura et al. (2019, PASJ, submitted) recently proposed a model based on thermal-viscous disk instability in a tilted disk to reproduce the IW And-type characteristics. IM Eri experienced the IW And-type phase in 2018 and we recorded three cycles of the (damping) oscillation phase terminated by brightening. We identified two periods during the IW And-type state: 4-5 d small-amplitude (often damping) oscillations and a 34-43 d long cycle. This behavior is typical for an IW And-type star. The object gradually brightened within the long cycle before the next brightening, which terminated the (damping) oscillation phase. This observation agrees with the increasing disk mass during the long cycle predicted by the Kimura et al. model of thermal-viscous disk instability in a tilted disk. We did not, however, succeed in detecting negative superhumps, which are considered to be the signature of a tilted disk.
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accretion, accretion disks,stars: dwarf novae,stars: individual (IM Eridani),stars: novae, cataclysmic variables
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要点】:本文研究了IM Eri在IW And型状态下的光学变光特性,通过观测数据和理论模型对比,验证了倾斜磁盘热粘滞不稳定性模型对IW And型星体的适用性。

方法】:使用光学观测方法对IM Eri在IW And型状态下的光变周期进行分析,并与Kimura等人的倾斜磁盘热粘滞不稳定性模型进行对比。

实验】:通过三次观测周期,记录了IM Eri在IW And型状态下的光学变光行为,使用的数据集为2018年的观测数据,实验结果显示了4-5天的小振幅振荡周期和34-43天的长周期,与模型预测相符,但未观测到负超凸现象。