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A comparison between the observed light curves of periodic masers inG9.62+0.20E and G188.95+0.89 and the results of a simple colliding-wind binarymodel is made to establish whether the flaring and other time-dependentbehaviour of the masers in these two star forming regions can be ascribed tochanges in the environment of the masers or in the continuum emission fromparts of the background \ion{H}{2} region. It is found that the light curves ofwidely different shape and amplitude in these two objects can be explainedwithin the framework of a periodic pulse of ionizing radiation that raises theelectron density in a volume of partially ionized gas against which the masersare projected. It is also shown that the decay of the 11.405 $\kmps$ maser inG188.95+0.89 can be explained very well in terms of the recombination of theionized gas against which the maser is projected while it would require veryspecial conditions to explain it in terms of changes in environment of themaser. We conclude that for G9.62+0.20E and G188.95+0.89 the observed changesin the masers are most likely due to changes in the background free-freeemission which is amplified by the masers.

On the methanol masers in G9.62+0.20E and G188.95+0.89