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Solar energetic particles acceleration by a shock wave accompanying a coronalmass ejection (CME) is studied. The description of the accelerated particlespectrum evolution is based on the numerical calculation of the diffusivetransport equation with a set of realistic parameters. The relation between theCME and the shock speeds, which depend on the initial CME radius, isdetermined. Depending on the initial CME radius, its speed, and the magneticenergy of the scattering Alfven waves, the accelerated particle spectrum isestablished during 10-60 minutes from the beginning of CME motion. The maximumenergies of particles reach 0.1-10 GeV. The CME radii of 3-5 $R_\odot$ and theshock radii of 5-10 $R_\odot$ agree with observations. The calculated particlespectra agree with the observed ones in events registered by ground-baseddetectors if the turbulence spectrum in the solar corona significantly differsfrom the Kolmogorov one.

Solar Energetic Particle Acceleration by a Shock Wave Accompanying a Coronal Mass Ejection in the Solar Atmosphere