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Fig. 6


Bolometric radiative intensity (left) and bolometric radiative flux (right) leaving the computational domain in the vertical direction through the top boundary as a function of time for both the magnetic (blue curve) and non-magnetic (red curve) solar model (G2V). The cyan and orange curves are the moving (box car) average of the magnetic and non-magnetic models, respectively, using a time window-width of 5000 s.

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