Gamma-rays from the Pulsar Wind Nebulae

Abstract

We estimate the gamma-ray fluxes expected from the northern sky pulsar wind nebulae (PWNe) applying time dependent hadronic-leptonic radiation model for the high energy processes inside the PWNe. This model base on the hypothesis, proposed by Arons and collaborators[1], which postulate that heavy nuclei are efficiently accelerated in the vicinity of young pulsars. We calculate the equilibrium spectra of leptons and hadrons at an arbitrary time after the pulsar formation. From normalization of the calculated synchrotron spectrum to the observed spectrum at low energies, the expected TeV gamma-ray fluxes from a population of the PWNe are estimated and its possible detectability by the future TeV telescopes is discussed.