  We describe a refined calculation of high energy emission from
rotation-powered pulsars based on the Outer Gap model of Cheng, Ho \&~Ruderman
(1986a,b). We have improved upon previous efforts to model the spectra from
these pulsars (e. g. Cheng, et al. 1986b; Ho 1989) by following the variation
in particle production and radiation properties with position in the outer gap.
Curvature, synchrotron and inverse-Compton scattering fluxes vary significantly
over the gap and their interactions {\it via} photon-photon pair production
build up the radiating charge populations at varying rates. We have also
incorporated an approximate treatment of the transport of particle and photon
fluxes between gap emission zones. These effects, along with improved
computations of the particle and photon distributions, provide very important
modifications of the model gamma-ray flux. In particular, we attempt to make
specific predictions of pulse profile shapes and spectral variations as a
function of pulse phase and suggest further extensions to the model which may
provide accurate computations of the observed high energy emissions.
