Physics – Nuclear Physics
Scientific paper
Feb 1981
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981azh....58..217r&link_type=abstract
(Astronomicheskii Zhurnal, vol. 58, Jan.-Feb. 1981, p. 217-220.) Soviet Astronomy, vol. 25, Jan.-Feb. 1981, p. 121, 122. Transl
Physics
Nuclear Physics
Gamma Ray Astronomy, Gamma Ray Spectra, Line Spectra, Nuclei (Nuclear Physics), Stellar Spectra, Supernova Remnants, Cosmic Plasma, Gamma Ray Bursts, Interstellar Matter, Milky Way Galaxy, Particle Collisions, Plasma-Particle Interactions, Shock Fronts, Stellar Envelopes, Stellar Evolution, Stellar Radiation
Scientific paper
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 epsilongamma is 0.8-6 MeV. Brightest lines are at the iron line when epsilongamma 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 epsilongamma is 0.845 MeV, is 1000 times weaker in quantum flux than the iron line where epsilonX 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.
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