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The Vela pulsar represents a distinct group of {\gamma}-ray pulsars. Fermi{\gamma}-ray observations reveal that it has two sharp peaks (P1 and P2) in thelight curve with a phase separation of 0.42 and a third peak (P3) in thebridge. The location and intensity of P3 are energy-dependent. We use the 3Dmagnetospheric model for the annular gap and core gap to simulate the{\gamma}-ray light curves, phase-averaged and phase-resolved spectra. We foundthat the acceleration electric field along a field line in the annular gapregion decreases with heights. The emission at high energy GeV band isoriginated from the curvature radiation of accelerated primary particles, whilethe synchrotron radiation from secondary particles have some contributions tolow energy {\gamma}-ray band (0.1 - 0.3 GeV). The {\gamma}-ray light curvepeaks P1 and P2 are generated in the annular gap region near the altitude ofnull charge surface, whereas P3 and the bridge emission is generated in thecore gap region. The intensity and location of P3 at different energy bandsdepend on the emission altitudes. The radio emission from the Vela pulsarshould be generated in a high-altitude narrow regions of the annular gap, whichleads to a radio phase lag of ~ 0.13 prior to the first {\gamma}-ray peak.

Gamma-ray Emission from the Vela Pulsar Modeled with the Annular Gap and Core Gap