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Fig. A.2

image

Bolometric light curves from HERACLES simulations for the RSG progenitor. At ~125 d, the shock between ejecta and progenitor wind leaves the grid and causes a slight glitch in the luminosity. In some models (e.g., RE3B7), the light curve shows a small bump at late times in the photospheric phase. This feature is associated with the dense shell that results from the dynamical influence of the magnetar power (even though we adopt a broad energy deposition profile; see Sect. 3). Models with a higher initial magnetar energy and/or a higher magnetar field tend to produce a more massive dense shell and show this late light curve bump.

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