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Fig. 10

image

Similar to Fig. 3, but now showing the influence of the 56Ni mixing on the SN radiation and gas properties at 300 d. The ejecta arises from a 20 M progenitor, weak mixing for all species, imposed H-rich envelope of 9 M, and a 56Ni mass of 0.08 M. An additional and variable amount of 56Ni mixing is applied increasing VNi from 750 (model 20-vni7p5e7) to 2500 km s−1 (model 20-vni2p5e8). With enhanced 56Ni mixing, more decay power is absorbed in the outer ejecta, causing a strengthening of Hα but a weakening of [Ca II] λλ 7291, 7323 because of the boost to the Ca ionization (the ionization shift also affects Fe I – II and Mg I lines in the optical and the near-infrared). (See Sect. 7 for discussion.)

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