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Late-time emission of the type II Supernovae powered by the radioactive decay56Ni−56Co−56Fe

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A one-zone model for the late time SN II energized by the radioactive decay56Ni−56Co−56Fe is presented. The model succeeds in reproducing for the late time evolution of Hα and [Oi] λ6300 emission lines in SN1970g for the reasonable set of parameters: mass of ejecta 4M , boundary velocityv 0=4000 km s−1 and amount of56NiM Ni=0.02M . However, a one-zone model does not account for the late time continuum. In the case of SN1980k the radioactive model fits Hα and [Oi] λ6300 emissions att≈250 day satisfactory but fails at very late time, e.g.,t=670 day when the predicted value of the ratioL(Hα)/L(6300) is two orders of magnitude smaller than the observed one. We suggest that the strong Hα emission in SN1980k on the 670th day is due to the interaction of the supernova envelope with the pre-SN wind. The radioactive model for the late time SN II predicts strong Mgii λ2800 line and detectable Hei λ10830 line in emission and absorption.

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Chugai, N.N. Late-time emission of the type II Supernovae powered by the radioactive decay56Ni−56Co−56Fe. Astrophys Space Sci 146, 375–388 (1988). https://doi.org/10.1007/BF00637587

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  • Time Evolution
  • Late Time
  • Emission Line
  • Time Continuum
  • Mgii