Abstract
By data obtained from investigations of hysteresis phenomenon in dependence of galactic cosmic ray intensity from solar activity we determine the change of cosmic ray density distribution in the Heliosphere during solar cycle in dependence of particle energy. On the basis of observation data and investigations of cosmic ray nonlinear processes in the Heliosphere we determine the space-time distribution of solar wind matter. Then we calculate the generation of gamma-rays by decay of neutral pions generated by nuclear interactions of modulated galactic cosmic rays with solar wind matter and determine the expected space-time distribution of gamma-ray emissivity. On the basis of these results we calculate the expected time variation of the angle distribution and spectra of gamma ray fluxes generated by interaction of modulated galactic cosmic rays with solar wind matter for local (inside the Heliosphere) and distant observers (for stellar winds).
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