  We consider a situation in which a pulsar is formed inside or close to a high
density region of a molecular cloud. Right after birth, the pulsar was very
active and accelerated hadrons and leptons to very high energies. Hadrons
diffuse through the supernova remnant (SNR) and some of them are trapped in the
nearby cloud interacting with the matter. We extend a recent time-dependent
model for the gamma-radiation of pulsar wind nebulae (PWNe) to describe this
more complicated astrophysical scenario. The example calculations have been
performed for two objects, IC443 and W41, which have recently been discovered
as sources of TeV gamma-rays. In this model the low energy TeV emission should
be correlated with the birth place of the pulsar and the region of dense soft
radiation rather than with its present position, provided that the injection
rate of relativistic particles into the PWNa has been much more efficient at
early times. The high energy TeV emission should be correlated with the
location of dense clouds which were able to capture high energy hadrons due to
their strong magnetic fields.
