We study the -ray emission properties of pulsars by using a new self-consistent outer gap model. The outer gap can exist in pulsars older than 1 million yr if the effect of magnetic inclination angle, as well as the average properties of the outer gap, are considered. The mature -ray pulsars, whose ages are between 0.3 and 3 million yr, are able to move up to high Galactic latitude. Moreover, their -ray luminosities are weaker, and their spectra are significantly softer than those of younger -ray pulsars in the Galactic plane. We use a Monte Carlo method to simulate the statistical properties of -ray pulsars in the Galaxy as well as in the Gould Belt. We find that -ray pulsars located at j b j< 5 and j b j > 5 have very different properties. High Galactic latitude -ray pulsars are dominated by mature pulsars with longer periods, weaker fluxes, and softer spectra. If the pulsar birth rates in the Galaxy and the Gould Belt are $10 À2 and $2 ; 10 À5 yr À1 , respectively, there are 42 and 35 radio-quiet -ray pulsars for j b j< 5 and j b j > 5 , respectively. The number of radio-quiet -ray pulsars from the Gould Belt are 2 and 13 for j b j< 5 and j b j > 5 , respectively. We suggest that a good fraction of unidentified EGRET -ray sources may be these radio-quiet -ray pulsars. Furthermore, -ray pulsars located at j b j > 5 satisfy L / L sd , whereas L / L sd for -ray pulsars in the Galactic plane, where $ 0:6 and $ 0:3, respectively.
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