We analyze time-series spectroscopy of the white dwarf merger candidate J005311 and confirm the unique nature of its optical spectrum. We detect an additional broad emission feature peaking at 343nm that was predicted in the Gvaramadze et al. (2019) models. Comparing ten spectra taken with the Large Binocular Telescope, we find significant variability in the profile of the strong O vi 381.1/383.4nm emission feature. This appears to be caused by rapidly shifting subpeaks generated by clumpiness in the stellar wind of J005311. This line variability is similar to what is seen in many Wolf-Rayet stars. However, in J005311, the rate of motion of the subpeaks appears exceedingly high as they can reach 16,000km s⁻¹ in less than two hours.

我们分析了白矮星合并候选者 J005311 的时间序列光谱，并确认了其光谱的独特性。我们检测到 Gvaramadze 等人预测的在 343nm 处达到峰值的额外宽发射特征。（2019）模型。比较用大型双筒望远镜拍摄的十个光谱，我们发现强 O vi 381.1/383.4nm 发射特征的轮廓存在显着变化 。这似乎是由 J005311 的恒星风中的团块产生的快速移动的子峰引起的。这种线变化类似于在许多 Wolf-Rayet 星中看到的变化。然而，在 J005311 中，次峰的运动速率显得异常高，因为它们可以在不到两个小时的时间内达到 16,000km s ^{-1 。}