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arXiv 2008.11871astro-ph.SRastro-ph.HE
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2018年WZ Sge型矮新星EG Cancri超爆发期间的多波长测光

Multi-wavelength photometry during the 2018 superoutburst of the WZ Sge-type dwarf nova EG Cancri

Mariko Kimura, Keisuke Isogai, Taichi Kato, Naoto Kojiguchi, Yasuyuki Wakamatsu, Ryuhei Ohnishi, Yuki Sugiura, Hanami Matsumoto, Sho Sumiya, Daiki Ito, Kengo Ni… 展开作者

Mariko Kimura, Keisuke Isogai, Taichi Kato, Naoto Kojiguchi, Yasuyuki Wakamatsu, Ryuhei Ohnishi, Yuki Sugiura, Hanami Matsumoto, Sho Sumiya, Daiki Ito, Kengo Nikai, Katsura Matsumoto, Sergey Yu. Shugarov, Natalia Kathysheva, Hiroshi Itoh, Pavol A. Dubovsky, Igor Kudzej, Hiroshi Akitaya, Kohei Oide, Takahiro Kanai, Chihiro Ishioka, Yumiko Oasa, Tonny Vanmunster, Arto Oksanen, Tamás Tordai, Katsuhiro L. Murata, Kazuki Shiraishi, Ryo Adachi, Motoki Oeda, Yutaro Tachibana, Seiichiro Kiyota, Elena P. Pavlenko, Kirill Antonyuk, Oksana Antonyuk, Nikolai Pit, Aleksei Sosnovskij, Julia Babina, Alex Baklanov, Koji S. Kawabata, Miho Kawabata, Tatsuya Nakaoka, Masayuki Yamanaka, Kiyoshi Kasai, Ian Miller, Stephen M. Brincat, Wei Liu, Mahito Sasada, Daisaku Nogami

备注：
Accepted for publication in PASJ. 13 pages and 9 figures
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摘要：

我们报告了2018年EG Cnc超级爆发的多波长测光。通过光学光度测量，我们探测到了A级超峰和持久的后期超峰，并限定了二元质量比及其可能的范围。质量比的中值为0.048，上限为0.057，这仍然意味着EG Cnc是周期弹跳器的可能候选者之一。该天体在这次超级爆发中还显示出多次再亮，尽管主超级爆发不同，但与1996- 1997年的前一次超级爆发相同。这意味着再亮类型是每个天体所固有的，并且与超级爆发开始时的初始盘质量无关。我们还发现，$B-I$和$J-K_{\rm S}$的颜色是不寻常的红色之前的再亮阶段，并成为蓝色的平静期间之间的再亮，这将意味着低温质量水库在最外层磁盘吸积后，随着时间的主要超级爆发。此外，紫外线通量和光通量一样对再亮敏感，在再亮阶段，$U-B$的颜色变得更红，这表明当该物体重复再亮时，内部圆盘变得更冷。因此，我们的研究结果基本上支持的想法，在最外层的磁盘冷质量库负责再亮。

英文摘要：

We report on the multi-wavelength photometry of the 2018 superoutburst in EG Cnc. We have detected stage A superhumps and long-lasting late-stage superhumps via the optical photometry and have constrained the binary mass ratio and its possible range. The median value of the mass ratio is 0.048 and the upper limit is 0.057, which still implies that EG Cnc is one of the possible candidates for the period bouncer. This object also showed multiple rebrightenings in this superoutburst, which are the same as those in its previous superoutburst in 1996--1997 despite the difference in the main superoutburst. This would represent that the rebrightening type is inherent to each object and is independent of the initial disk mass at the beginning of superoutbursts. We also found that $B-I$ and $J-K_{\rm S}$ colors were unusually red just before the rebrightening phase and became bluer during the quiescence between rebrightenings, which would mean that the low-temperature mass reservoir at the outermost disk accreted with time after the main superoutburst. Also, the ultraviolet flux was sensitive to rebrightenings as well as the optical flux, and the $U-B$ color became redder during the rebrightening phase, which would indicate that the inner disk became cooler when this object repeated rebrightenings. Our results thus basically support the idea that the cool mass reservoir in the outermost disk is responsible for rebrightenings.

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