Production and propagation of high-energy solar cosmic rays

The processes of production and propagation of high-energy solar cosmic ray (SCR) protons are studied. For these purposes the experimental data obtained at neutron monitors (NM) and satellites are used, as well as the results of numerical solutions of the equation of flare-accelerated particle propagation. The generation of particles with the energy ∼ 10-100 GeV takes place during flares in the Sun. The drift of high-energy SCR has a considerable effect on space-time intensity and anisotropy characteristics of high-energy SCR protons. A considerable transformation of SCR energy spectrum shape can take plce during the propagation of flare SCR from the source to the point of their detection. The absence of noticeable fluxes of low-energy particles during small counting rate increase in NM from SCR is explained by the drift mechanism when practically complete separation of low-energy and high-energy components is observed