  We estimate the TeV gamma-ray fluxes expected from the population of young
pulsars in terms of the self-consistent time dependent hadronic-leptonic model
for the high energy processes inside the pulsar wind nebulae. This radiation
model bases on the hypothesis of Arons and collaborators who postulate that
leptons are accelerated inside the nebulae as a result of resonant scattering
on heavy nuclei, which in turn are accelerated in the pulsar wind region or the
pulsar inner magnetosphere. Our aim is to find out which nebulae on the
nortehrn hemisphere are the best candidates for detection at energies above 60
GeV and 200 GeV by the next generation of low threshold Cherenkov telescopes.
