  An extensive program for the calculation of galactic cosmic-ray propagation
has been developed. Primary and secondary nucleons, primary and secondary
electrons, secondary positrons and antiprotons are included. Fragmentation and
energy losses are computed using realistic distributions for the interstellar
gas and radiation fields.
  Models with diffusion and convection only do not account naturally for the
observed energy dependence of B/C, while models with reacceleration reproduce
this easily. The height of the halo propagation region is determined, using
recent 10Be/9Be measurements, as greater than 4 kpc. The radial distribution of
cosmic-ray sources required is broader than current estimates of the SNR
distribution for all halo sizes. Our results include an estimate of cosmic-ray
antiproton and positron spectra, and the Galactic diffuse gamma-ray emission
(see accompanying paper: Moskalenko 1998b).
