  We argue that the periodic variability of Class II methanol masers can be
explained by variations of the dust temperature in the accretion disk around
proto-binary star with at least one massive component. The dust temperature
variations are caused by rotation of hot and dense material of the spiral shock
wave in the disk central gap. The aim of this work is to show how different can
be the Class II methanol maser brightness in the disk during the Moment of
Maximum Illumination by the Spiral Shock material (hereafter MMISS) and the
Moment when the disk is Illuminated by the Stars Only (MISO). We used the code
CLOUDY (v13.02) to estimate physical conditions in the flat disk in the MISO
and the MMISS. Model physical parameters of the disk were then used to estimate
the brightness of 6.7, 9.9, 12.1 and 107 GHz masers at different impact
parameters $p$ using LVG approximation. It was shown that the strong masers
experience considerable brightness increase during the MMISS with respect to
MISO. There can happen both flares and dips of the 107 GHz maser brightness
under the MMISS conditions, depending on the properties of the system. The
brightest 9.9 GHz masers in the MMISS are situated at the greater $p$ than the
strong 6.7, 12.1 and 107 GHz masers that are situated at $p<200$ AU. The
brightness of 9.9 GHz maser in the MMISS suppressed at $p<200$ AU and increase
at $p>200$ AU.
