An explanation of variable peculiarities in spectra of electrons and positrons of cosmic rays

It is shown that the excesses in the sum of fluxes (e ⁺ + e ^?) in cosmic rays in the energy range (10–1000) GeV and in the flux ratio e ⁺/(e ⁺ + e ^?) in the range > 10 GeV, observed both in recent and old experiments, can be explained by an accelerator of charged particles operating on the heliosphere periphery, in the region beyond the termination shock of the solar wind (～100 AU). Variations in the value and position of peculiarities in the spectra (e ⁺ + e ^?), as well as increasing ratio of fluxes e ⁺/(e ⁺ + e ^?), can be associated with variations of solar activity (and, as a consequence, of acceleration regimes) on different phases of the 11-years solar cycle. The results of numerical simulation of capture and acceleration of charged particles by packets of plasma waves in the heliospheric magnetic field are presented.