Comparison of models RE0p4B3p5 and RE0p4B3p5d to test the influence of the radial profile used for the deposition of magnetar power. Ordered clockwise from top left, we show the radial variation of the mass density, temperature, local emissivity from magnetar power, and the cumulative kinetic energy integrated outward from the inner boundary, all at 116 d after the start of the HERACLES simulation. Model RE0p4B3p5 spreads the magnetar energy over a large range of masses, while model RE0p4B3p5d deposits all the magnetar energy over the inner 0.1 M⊙.
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