Nuclear gamma-ray lines from supernova remnants

Possible fluxes and intensities of certain gamma-ray lines from young supernova remnants are calculated within the framework of a remnant model by Chevalier (1977) and Shklovskii (1976). Estimates show that the total flux in gamma-ray lines from the 1181 supernova, for example, does not exceed 0.0001 photon/sq cm-sec, where epsilon_gamma is 0.8-6 MeV. Brightest lines are at the iron line when epsilon_gamma is 0.845 MeV, and where the flux is on the order of 0.00002 photon/sq cm-sec. A comparison also shows that the gamma-ray line from remnants, where epsilon_gamma is 0.845 MeV, is 1000 times weaker in quantum flux than the iron line where epsilon_X is 6.8 keV. All estimates assume that the interstellar medium around the supernovae and the active regions of Seyfert galaxies have the normal abundance of elements.