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Fig. 1.


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Emergence of the convection magnetic flux tube into the solar atmosphere at t = 110 t 0 for both the stable SD (A) and the unstable SD E (B) simulations. The cyan lines trace the coronal arcade magnetic field, originating from the lower boundaries, whereas the red lines belong to the magnetic flux tube and originate from the y = ±maxy side boundaries. The gray scale indicates the magnetic field strength at the surface.

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