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For great solar FEP events Etot = 10 ■ 10 erg , and more (see in Dorman, M1957, M1963a,b, M1978; Dorman and Miroshnichenko, M1968; Dorman and Venkatesan, 1993; Stoker, 1995; Miroshnichenko, M2001), for great stellar FEP

events Etot ~ 1035 ■ 1037 erg (see in Gershberg and Shakhovskaya, 1983; Korotin and Krasnobaev, 1985; Gershberg et al., 1987; Kurochka, 1987). In Eq. 1.13.1

is the diffusion coefficient, A, (Ek) is the transport path for particle scattering in the interplanetary space, v(Ek) is the particle velocity as a dependence on the kinetic energy per nucleon Ek :

where mnc is the rest energy of the nucleon. According to numeral experimental data and theoretical investigations A , (E^) have a bride minimum in the region 0.10.5 GeV/nucleon and increases with energy decreasing lower than this region at about ^ E- (caused by 'tunnel' effect for particles with curvature radius in the interplanetary magnetic field smaller than the smallest scale of hydromagnetic turbulence, see in Dorman, M 1975a) as well as with energy increasing over this interval as ^ E^, where ¡5 depends from the spectrum of turbulence and usually increases from 0 up to about 1 for high energy particles of few GeV/nucleon and then up to about 2 for very high energy particles with curvature radius in IMF bigger than biggest scale of magnetic inhomogeneities in IMF (according to investigations of galactic cosmic ray modulation in the Heliosphere it will be at Ek > 20 -30 GeV/nucleon). For calculations of expected space-time distribution of gamma ray emissivity we try to describe this dependence for the most part of spectrum what is important for gamma ray emission (from about 0.01 GeV/nucleon up to about 20 GeV/nucleon) approximately as

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