By using the surface features as an indication of magnetic field strength in Pre Main Sequence (PMS) stars, using the LCOGT network, a long-term photometric monitoring campaign with semi-regular cadence will allow one to measure magnetic activity cycles. As the surface features get more prevalent and then disappear, the amplitude of the brightness modulation they create will increase and decrease. The period of this amplitude variation should be a good proxy for magnetic field activity.
The period of magnetic field cycles of young PMS stars is thus far largely unexplored because of the time involved (the Sun's cycle is about 11 years) and the kind of data necessary. LCOGT will be perfect for this sort of observation. Many clusters can be put in the queue with low priority and observed whenever a telescope is idle. Over several years, a sufficient data set for this project can be collected without disrupting any other observations.