arXiv 0904.34252009-04-22astro-ph.SR

2007年天秤座超级爆发期间WZ Sge型矮新星GW的光谱观测

Spectroscopic Observations of the WZ Sge-Type Dwarf Nova GW Librae during the 2007 Superoutburst

Kazuo Hiroi, Daisaku Nogami, Yoshihiro Ueda, Yuuki Moritani, Yuichi Soejima, Akira Imada, Osamu Hashimoto, Kenzo Kinugasa, Satoshi Honda, Shin-ya Narusawa, Mako… 展开作者

Kazuo Hiroi, Daisaku Nogami, Yoshihiro Ueda, Yuuki Moritani, Yuichi Soejima, Akira Imada, Osamu Hashimoto, Kenzo Kinugasa, Satoshi Honda, Shin-ya Narusawa, Makoto Sakamoto, Ryo Iizuka, Kentaro Matsuda, Hiroyuki Naito, Takashi Iijima, Mitsugu Fujii

备注：: 10 pages, 9 figures, accepted for publication in PASJ
DOI：: 10.1093/pasj/61.4.697

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摘要：

在2007年的超级爆发期间，我们对矮新星GW Librae（GW Lib）进行了国际光谱观测活动。我们的观测周期涵盖了超级爆发的上升阶段，最大值，缓慢衰减阶段（高原），以及从高原快速下降后的长衰落尾巴。在观测过程中，光谱特征发生了显著变化。在上升相中，仅存在H $α$、H $β$和H $γ$的吸收线。在最大值附近，光谱显示出H $α$、He I 5876、He I 6678、He II 4686和C III/N III的单峰发射线以及Balmer组分和He I的吸收线。这些发射线在平台期的后半部分显著减弱。在衰落的尾部，所有的巴耳末线和He I 6678都在发射中，正如在静止时所观察到的那样。我们发现H $α$发射分量的中心在整个轨道相位上是稳定的，这与系统的低倾角是一致的。通过与2001年超爆发期间的WZ Sge（与GW Lib同类型的大倾角恒星）的观测结果比较，我们解释了H $α$轮廓在衰落尾相之前的变化是由于白矮星和内盘辐射在吸积盘外缘形成的光电离区。

英文摘要：

We carried out an international spectroscopic observation campaign of the dwarf nova GW Librae (GW Lib) during the 2007 superoutburst. Our observation period covered the rising phase of the superoutburst, maximum, slowly decaying phase (plateau), and long fading tail after the rapid decline from the plateau. The spectral features dramatically changed during the observations. In the rising phase, only absorption lines of H$α$, H$β$, and H$γ$ were present. Around the maximum, the spectrum showed singly-peaked emission lines of H$α$, He I 5876, He I 6678, He II 4686, and C III/N III as well as absorption lines of Balmer components and He I. These emission lines significantly weakened in the latter part of the plateau phase. In the fading tail, all the Balmer lines and He I 6678 were in emission, as observed in quiescence. We find that the center of the H$α$ emission component was mostly stable over the whole orbital phase, being consistent with the low inclination of the system. Comparing with the observational results of WZ Sge during the 2001 superoutburst, the same type of stars as GW Lib seen with a high inclination angle, we interpret that the change of the H$α$ profile before the fading tail phase is attributed to a photoionized region formed at the outer edge of the accretion disk, irradiated from the white dwarf and inner disk.

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