Abstract
Abstract Using a simple accelerating model and an assumption that γ-rays originate from p–p collisions for a π0 model, we investigate γ-ray sources like V407 Cygni in symbiotic stars. The upper limit of their occurrence rate in the Galaxy is between 0.5 and 5 yr−1, indicating that they may be important sources of high-energy γ-rays. The maximum energies of the accelerated protons mainly distribute around 1011eV, and barely reach 1015eV. The novae occurring in D-type SSs with ONe white dwarfs and long orbital periods are good candidates for γ-ray sources. Due to a short orbital period which results in a short acceleration duration, the nova occurring in symbiotic star RS Oph cannot produce γ-ray emission like that in V407 Cygni.
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