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arXiv 0912.4938astro-ph.SR
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太阳通量浮现模拟

Solar Flux Emergence Simulations

R. F. Stein, A. Lagerfjärd, Å. Nordlund, D. Georgobiani

备注：
Solar Physics (in press), 12 pages, 13 figure
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摘要：

我们模拟上升通过上层对流区和出现通过太阳表面的初始均匀，无扭曲，水平磁通量与相同的熵的非磁性等离子体，平流到一个域48毫米宽，从20毫米深。磁场被发散的上升气流向上平流输送，并在下降气流中被向下拉，这产生了一个层次的环状结构，随着接近表面，其规模越来越小。在20 μ m深度处，10 kG强度的场与20或40 kG强度的场之间的行为有显著差异。10 kG的磁场对对流流的影响很小，并且显示出很小的磁浮力效应，在典型的流体上升时间内从20 Mm深度32小时到达表面。20和40 kG的磁场显著地改变了对流，导致上升流体的细长单元与磁场对齐，并且它们的磁浮力使它们比流体上升时间更快地上升到表面。20 kG的磁场产生一个大规模的磁回路，当它通过表面出现时，导致形成双极孔状结构。

英文摘要：

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 non-magnetic plasma that is advected into a domain 48 Mm wide from from 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 little 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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