  Thousands of ring-like bubbles appear on infrared images of the Galaxy plane.
Most of these infrared bubbles form during expansion of HII regions around
massive stars. However, the physical effects that determine their morphology
are still under debate. Namely, the absence of the infrared emission toward the
centres of the bubbles can be explained by pushing the dust grains by stellar
radiation pressure. At the same time, small graphite grains and PAHs are not
strongly affected by the radiation pressure and must be removed by another
process. Stellar ultraviolet emission can destroy the smallest PAHs but the
photodestruction is ineffective for the large PAHs. Meanwhile, the stellar wind
can evacuate all types of grains from HII regions. In the frame of our
chemo-dynamical model we vary parameters of the stellar wind and illustrate
their influence on the morphology and synthetic infrared images of the bubbles.
