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Paper: Emerging Flux Simulations
Volume: 454, The 3rd Hinode Science Meeting
Page: 193
Authors: Stein, R. F.; Lagerfjärd, A.; Nordlund, Å; Georgobiani, D.
Abstract: We simulate the rise through the upper convection zone and emergence through the solar surface of initially uniform, untwisted, horizontal magnetic flux that is advected into a domain 48 Mm wide by 20 Mm deep, with the same entropy as the non-magnetic plasma. The magnetic field is transported upward by the diverging upflows and pulled down in the downdrafts, which produces a hierarchy of loop-like structures of increasingly smaller scale as the surface is approached. 20 kG fields at the bottom significantly modify the convective flows, leading to long thin cells of ascending fluid aligned with the magnetic field. Their magnetic buoyancy makes them rise to the surface faster than the fluid rise time. A large scale magnetic loop is produced that, as it emerges through the surface, leads to the formation of a bipolar pore-like structure.
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