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An extensive program for the calculation of galactic cosmic-ray propagationhas been developed. This is a continuation of the work described in Strong &Youssefi (1995). The main motivation for developing this code is the predictionof diffuse Galactic gamma rays for comparison with data from the CGROinstruments EGRET, COMPTEL, and OSSE. The basic spatial propagation mechanismsare (momentum-dependent) diffusion, convection, while in momentum space energyloss and diffusive reacceleration are treated. Primary and secondary nucleons,primary and secondary electrons, and secondary positrons are included.Fragmentation and energy losses are computed using realistic distributions forthe interstellar gas and radiation fields.  This study indicates that it is possible to construct a model satisfying awide range of observational constraints and provides a basis for futuredevelopments.

Modelling cosmic rays and gamma rays in the Galaxy