2019MNRAS.485.2759V

Since the discovery of periodic class II methanol masers at 6.7 and 12.2 GHz associated with high-mass star formation regions (HMSFRs), a number of possible driving mechanisms have been proposed to explain this phenomenon. Here, we apply a more realistic treatment of the original colliding wind binary (CWB) model explanation to investigate to what extent it can describe the flare profiles of the periodic methanol masers. It was found that the CWB hypothesis is feasible from an energetics standpoint, because the emission from the shocked gas does cause an outward shift of the position of the ionization front (IF). This confirms that the energy budget available from the shocked gas is enough to be the driving force behind the CWB model. The CWB model describes the light curve of the 1.25 km s^–1 12.2 GHz velocity feature of G9.62 + 0.20E very well over 4000 d. The quiescent state flux density of the 1.25 km s^–1 velocity feature can also be described very well by the time-dependent change in electron density (n_e). The CWB model also describes the other periodic methanol masers, G22.357 + 0.066, G37.55 + 0.20, and G45.473 + 0.134, which have similar light curves, very well. This strongly suggests that these periodic methanol masers can be described by the time-dependent change in the free-free emission from some part of the background H II region against which the masers are projected.