  We present 24 micron images of three protoplanetary disks being
photoevaporated around high mass O type stars. These objects have ``cometary''
structure where the dust pulled away from the disk by the photoevaporating flow
is forced away from the O star by photon pressure on the dust and heating and
ionization of the gas. Models of the 24 micron and 8 micron brightness profiles
agree with this hypothesis. These models show that the mass-loss rate needed to
sustain such a configuration is in agreement with or somewhat less than the
theoretical predictions for the photoevaporation process.
