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Fig. 11

image

Similar to Fig. 3, but now showing the influence of the 56Ni mass on the SN radiation (for better visibility, a logarithmic scale is used for the luminosity). The ejecta arises from a 20 M progenitor, weak mixing for all species, no additional mixing of 56Ni, imposed H-rich envelope of 9 M, and is characterized by a 56Ni mass of 0.004, 0.02, 0.08, 0.16, and 0.32 M. A greater 56Ni mass boosts the electron density and species ionization, inhibits forbidden line emission (in favor instead, for example, of recombination lines), and strengthens optical depth effects and continuum processes (primarily in association with electron scattering). (See Sect. 8 for discussion.)

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