Gamma-Rays and Neutrinos from Very Young Supernova Remnants

We consider the result of acceleration of heavy ions in the slot gap potential of a very young pulsar with a hot polar cap. Photodisintegration of the heavy ions in the radiation field of the polar cap and pulsar surface gives rise to a flux of energetic neutrons. Some fraction of these neutrons interact with target nuclei in the supernova shell to produce a prompt neutrino and gamma-ray signal. Neutrons that do not interact promptly travel far from the pulsar where they decay into protons which await the arrival of target nuclei in the supernova shell, and then produce a delayed neutrino and gamma-ray signal. The TeV neutrino and 100 MeV and TeV gamma-ray signals should be observable from very young supernova remnants in our galaxy for a range of pulsar parameters.