Scientific impact
Figure three from Chené & St-Louis (2010) representing photometric lightcirves from their observations of WR 1 folded with a 16.9 day and 8.4 day period, respectively.

Morel et al. 1999, ApJ, 518, 428 ("A 2.3 Day Periodic Variability in the Apparently Single Wolf-Rayet Star WR 134: Collapsed Companion or Rotational Modulation?") have found a coherent 2.25+/-0.05 day periodicity in the line-profile changes of He II 4686, although the global pattern of variability is different from one epoch to another. The same period has been (marginally) found in UBV photometry. This makes it one of the three WR stars (with WR1 (Chené & St-Louis 2010, ApJ, 716, 929) and WR6 (Morel et al. 1997, ApJ, 482, 470)) for which large scale spectral variations, likely to be caused by the presence of CIRs in the wind, have been observed. However, since then, WR 134 has never been monitored a second time. Hence, it would be valuable to confirm the currently known period and variability pattern.

Moreover, none of these three WR star showing CIR has been monitored on a very long time interval in spectroscopy. Such a monitoring would give us information on the epoch dependency, the long term variability pattern and the evolution of the period, if there is any. Also, it would be very interesting to look for a periodicity in the epoch dependency; it would give us invaluable information on the origin of CIRs (would it by magnetic field activity at the surface, stellar pulsations or something else)! Such study has never been done yet, since none of the previous spectroscopic campaign has been covering more than a month (contiguously).