1996A&AS..120C.167L

We report the development of a computer code that solves the coupled particle and photon kinetic equations, for explaining the emissions from tens of keV to several MeV from galactic black hole candidates observed with the COMPTEL and OSSE experiments on the Compton Gamma-Ray Observatory. Specifically, we examine the role of stochastic particle acceleration from wave-particle resonant interactions in the accreting plasma. This process has been treated as diffusion (in momentum) and systematic acceleration in the particle's Fokker-Planck equation. Pair production, annihilation, radiative cooling and escape have also been included. We show that electrons can be accelerated beyond the thermal distribution to form a new population - a ``bump'' in the tail. Radiation by inverse Compton scattering off the thermal (from the background) and non-thermal (produced by acceleration) particles can in principle explain the hard X-ray to gamma-ray emissions from black hole candidates. We present model fits of Cyg X-1 and GRO J0422 in the 50keV-5MeV region observed with OSSE and COMPTEL.