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Fig. 21.


Bolometric light curves for models r0e2 and r0e2ba, which differ only in magnetar field strength. The thin solid and dashed lines correspond to the instantaneous magnetar power absorbed by each ejecta. The contribution from 0.13 M of 56Ni is in part responsible for the offset after 100 d. This offset is small in the model r0e2ba due to the much greater magnetar power at late times.

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