[en] Assuming that pulsar γ-rays are produced via curvature radiation of primary electrons near the neutron star and that they are attenuated only through the pair production process in strong electric and magnetic fields, we use a detailed model of the magnetosphere to calculate the resulting optical depths and pulse shapes. We consider both the effect of E.B=0 and E.Bnot =0 on the attenuation of the photons, and the effect of photon energy, rotation rate, and obliquity on the pulse shapes. It is found that pulsar rotation tends to increase pair production, causing large optical depths for the shortest period pulsars. The calculations also predict high-energy cutoffs and spectra for the observable γ-ray emission