The expected gamma ray emissivity distribution from the interaction of «-particles with solar wind matter will be determined by introducing Eq. 1.14.9-1.14.12, Eq. 1.13.15 in Eq. 1.14.14 and then in Eq. 1.14.15:

Ek min iEn)

For the radial extended of solar or stellar wind the space-time distributions of gamma ray emissivity according to Eq. 1.14.16 will be mainly determined by the function

where F^ (ey) is the emissivity spectrum from galactic CR protons in the interstellar space (as background emissivity from interstellar matter with density no according to Dermer, 1986a,b), and n (0, t) is the density of solar or stellar wind on the latitude 0 on the distance r1 = 1 AU from the star. In Eq. 1.14.18

and (RYfi)ef (e y) is some effective value of RY fi for particles responsible for gamma ray generation with energy Ey. According to Dermer (1986a,b) the expected gamma ray emissivity from all particles in galactic CR F Y (ey , r, t) will increase in about 1.45 times if we take into account also a- particles and heavier particles in galactic CR:

FY ((, r, t ) = 1.45FPH (( /0 [1 - yo]"'( r]V - Ä(E , t / -

1.14.5. Expected angular distribution of gamma ray fluxes from solar wind

Let us assume that the observer is inside the Heliosphere, at a distance ro^s < ro from the Sun and at a helio-latitude #obs. We can determine the line of sight of observation by the angle 0[s, computed from the equatorial plane from the anti-Sun direction to the North. In this case the expected angular distribution and time variations of gamma ray fluxes for a local observer from interaction of galactic CR with solar wind matter will be

O Y Er,r>bsA,t)= 1.45x JdLFpH (r,LEobsA),t).(1.14.21)

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