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Fig. 3


Bolometric light curves computed with HERACLES for models RE0p4B3p5 (homogenous composition with Ā = 1.35) and RE0p4B3p5x (chemically stratified and spanning Ā = 1.35 up to 17).Allowing for a depth dependent abundance only affects the light curve after maximum, when the former (metal-rich) He-core material is progressively revealed. The impact on the light curve is however minor here. The glitch at 125 d occurs when the outer shock with the progenitor wind leaves the Eulerian grid at 1016 cm. The spectra for these two models at maximum light are identical (hence not shown). This is because the spectrum then forms within the H-rich layers, and thus at the same composition in both models.

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