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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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