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Fig. 15


Evolution with SN age of the Hα luminosity (top and middle) or the normalized Hα luminosity (bottom) for a subset of models covering stripped material masses of about 0.0018 (blue), 0.018 (red), and 0.18 M (yellow). For the two lower panels, the Hα flux is calculated by integrating over Hα after subtracting the flux from the corresponding reference model with Mst = 10−5 M. For the top panel, the Hα flux is calculated from the H I spectrum. The different behavior with stripped material masses arises from optical depth effects, which are important in the time span 100–200 d here. These effects can produce an Hα luminosity that evolves very differently from that expected for 56Co decay, even though 56Co decay is the powersource for the emission from the stripped material.

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