In the HE/VHE regimes, the Fermi, VERITAS and MAGIC experiments have detected pulsed signals from the Crab pulsar upto 400 GeV. The light curves and the spectra obtained from the Crab and other rotation-powered pulsars, suggest that the gamma-ray pulsars have high-altitude emission zones, which avoid super-exponential cutoff due to magnetic pair production and reproduce wide-separated double-peak light curves.

I thus examine the outer-magnetospheric emission model and analytically demonstrate that their gamma-ray luminosity is naturally proportional to the square root of the spin-down luminosity, which is consistent with the Fermi observations. I further confirm this analytical prediction by numerically solving the emission zone of typical pulsars from the set of Maxwell and Boltzmann equations. Finally, I show that young pulsars with ages around 3000 years exhibit relatively strong, pulsed, inverse-Compton emission component in 0.3-10 TeV, and discuss their detectability with the current and future ground-based Imaging Air Cherenkov Telescopes.