Abstract
On the basis of investigations of solar flare energetic particle (FEP) generation and propagation, we calculate the expected gamma ray emissivity from interaction of FEP with stellar wind matter. Then we estimate the expected gamma ray flux from different directions and its change with time. We use the obtained for rough estimations of expected gamma ray fluxes in energy range 0.1GeV-TeV from FEP interaction with wind matter on different types of stars.
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