  Using the first three and a half years of observations from the Energetic
Gamma Ray Telescope (EGRET) on board the Compton Gamma Ray Observatory (CGRO),
phase-resolved analyses are performed on the emission from the three brightest
high-energy gamma-ray pulsars, Crab, Geminga, and Vela. For each pulsar, it is
found that there is detectable high-energy gamma-ray emission above the
galactic diffuse background throughout much of the pulsar rotation cycle. A
hardness ratio is introduced to characterize the evolution of the spectral
index as a function of pulsar phase. While the hardest emission from the Crab
and Vela pulsars comes from the bridge region between the two gamma-ray peaks,
the hardest emission from Geminga corresponds to the second gamma-ray peak. For
all three pulsars, phase-resolved spectra of the pulse profile components
reveal that although there is a large variation in the spectral index over the
pulsar phase interval, the high-energy spectral turnover, if any, occurs at
roughly the same energy in each component. The high-energy gamma-ray emission
from the Crab complex appears to include an unpulsed ultra-soft component of
spectral index ~ -4.3 which dominates the total emission below 100 MeV. This
component is consistent with the expected emission from the tail end of the
Crab nebula synchrotron emission.
