The Astrophysical Journal
The American Astronomical Society
The gamma-ray luminosity of a typical type I supernova remnant has been calculated by assuming that the origin of the optical luminosity is due to the energy of the radioactive decay of Ni56. Tt is ex- pected that Ni56 is the most abundant nucleus resulting from silicon burning in the supernova shock conditions. The requisite mass of Ni56 (0.14 Mo) gives rise to gamma-ray lines with energies near 1 MeV that should be detectable in young supernova remnants at distances up to a few Mpc. Future detectors aboard satellites should be able to detect events at the rate of about two observable events per year. A few supernova remnants in the Galaxy should be observable at all times in lines following the decay of Ti44.
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