  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; arXiv:1904.00012) models. Comparing ten spectra taken
with the Large Binocular Telescope (LBT), we find significant variability in
the profile of the strong OVI 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 16000 km/s in less than two hours.
