Solar Flux Emergence Simulations |
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| Authors: | R F Stein A Lagerfjärd Å Nordlund D Georgobiani |
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| Institution: | (1) HAO, National Center for Atmospheric Research, Boulder, CO, USA |
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| Abstract: | We simulate the rise through the upper convection zone and emergence through the solar surface of initially uniform, untwisted,
horizontal magnetic flux, with the same entropy as the nonmagnetic plasma, that is advected into a domain 48 Mm wide by 20 Mm
deep. The magnetic field is advected 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. There are significant differences between
the behavior of fields of 10 kG and 20 or 40 kG strength at 20 Mm depth. The 10 kG fields have little effect on the convective
flows and show small magnetic-buoyancy effects, reaching the surface in the typical fluid rise time from 20 Mm depth of 32
hours. 20 and 40 kG fields significantly modify the convective flows, leading to long, thin cells of ascending fluid aligned
with the magnetic field and their magnetic buoyancy makes them rise to the surface faster than the fluid rise time. The 20 kG
field produces a large-scale magnetic loop that as it emerges through the surface leads to the formation of a bipolar, pore-like
structure. |
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