  We investigate particle accelerators in rotating neutron-star magnetospheres,
by simultaneously solving the Poisson equation for the electrostatic potential
together with the Boltzmann equations for electrons, positrons and photons on
the poloidal plane. Applying the scheme to the three pulsars, Crab, Vela and
PSR B1951+32, we demonstrate that the observed phase-averaged spectra are
basically reproduced from infrared to very high energies. It is found that the
Vela's spectrum in 10-50 GeV is sensitive to the three-dimensional magnetic
field configuration near the light cylinder; thus, a careful argument is
required to discriminate the inner-gap and outer-gap emissions using a
gamma-ray telescope like GLAST. It is also found that PSR B1951+32 has a large
inverse-Compton flux in TeV energies, which is to be detected by ground-based
air Cerenkov telescopes as a pulsed emission.
