  Shock waves associated with shell type supernova remnants are considered to
be possible sites of cosmic ray acceleration. Since shocks are capable of
accelerating electrons in addition to protons one anticipates both species to
contribute to the high energy radiation expected from these objects. Adopting a
simple model for particle acceleration we calculate in a self-consistent manner
the time-dependent synchrotron and inverse Compton radiation of high energy
electrons assumed either to be accelerated directly by the shock wave or to be
injected at high energies as secondaries from the hadronic collisions of
relativistic protons with the circumstellar material. We deduce that for
standard supernova parameters the TeV flux produced from neutral pion decay is
about the same order as the flux expected from directly accelerated electrons.
