2010年爆发期间，类共生周期新星天鹅座V407的光谱演化。II。星周环境及其后果
The spectroscopic evolution of the symbiotic-like recurrent nova V407 Cygni during its 2010 outburst. II. The circumstellar environment and the aftermath
摘要：
天鹅座V407在2010年3月10日的新星爆发是这颗恒星的第一次观测，但它与著名的共生型复发新星RS Oph的相似之处表明它也是这种罕见类型的银河系新星的成员。这颗新星是第一个在$γ$射线能量下被探测到的新星，也是该系统中第一个已知的新星爆炸。这种爆发的广泛的多波长覆盖范围使其成为与类似系统已知的少数其他爆发的理想比较。我们扩展我们以前的分析，从爆炸的米拉和扩大冲击详细的时间发展的光电离的米拉风，拱星介质，和冲击拱星环境，推导出它们的物理参数，以及它们如何与环境的大尺度结构，扩展以前的覆盖面超过500天后爆发。在Mira风中形成的Fe峰离子的吸收线在第69天之前的低速下可见为P Cyg轮廓，大约在X射线峰的时间，我们确定了许多吸收跃迁，而没有伴随金属线的发射。在2010年观察期间，H Balmer线显示出较强的P Cyg吸收谷，该吸收谷在第128天减弱。我们区分的冲击，光电离环境，色球层和内米拉风爆发后超过一年采取的光谱的组件。多壳层和辐射激发现象与最近引用的GRB和SNIa（严重截断）相似。
英文摘要：
The nova outburst of V407 Cyg in 2010 Mar. 10 was the first observed for this star but its close resemblance to the well known symbiotic-like recurrent nova RS Oph suggests that it is also a member of this rare type of Galactic novae. The nova was the first detected at $γ$-ray energies and is the first known nova explosion for this system. The extensive multiwavelength coverage of this outburst makes it an ideal comparison with the few other outbursts known for similar systems. We extend our previous analysis of the Mira and the expanding shock from the explosion to detail the time development of the photoionized Mira wind, circumstellar medium, and shocked circumstellar environment to derive their physical parameters and how they relate to large scale structure of the environment, extending the previous coverage to more than 500 days after outburst. Absorption lines of Fe-peak ions formed in the Mira wind were visible as P Cyg profiles at low velocity before Day 69, around the time of the X-ray peak and we identified many absorption transitions without accompanying emission for metal lines. The H Balmer lines showed strong P Cyg absorption troughs that weakened during the 2010 observing period, through Day 128. We distinguish the components from the shock, the photoionized environment, and the chromosphere and inner Mira wind using spectra taken more than one year after outburst. The multiple shells and radiative excitation phenomenology are similar to those recently cited for GRBs and SNIa (severely truncated)
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