Supergranule Scale Flux Emergence Simulations

Details Supergranule Scale Flux Emergence Simulations Supergranule Scale Flux Emergence Simulations

May 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21621103s&link_type=abstract

American Astronomical Society, AAS Meeting #216, #211.03; Bulletin of the American Astronomical Society, Vol. 41, p.866

Astronomy and Astrophysics

Astronomy

1

Scientific paper

We simulate the rise of initially horizontal, untwisted magnetic flux from 20 Mm depth through the near surface convection to the solar surface in a domain 48 Mm wide. The magnetic field is transported upward by diverging upflows aided by magnetic buoyancy, and pushed down by downdrafts, which produces a hierarchy of loop like structures, of increasingly smaller scale as the surface is approached. We compare two cases with field strengths of 5 and 20 kG at 20 Mm depth. In the stronger field strength case, the magnetic field significantly disturbs the convection below 3 Mm, inhibiting the vertical motion, shutting off convective energy transport and producing elongated cellular structures in the field direction. Shallower than 3 Mm the convection appears normal, but with concentrated vertical magnetic concentrations ("flux tubes") extending through the surface and producing pores where the field is greatest. Even in the weaker field case, the magnetic field inhibits vertical motions and the convective transport of energy although the convective cellular pattern is not significantly distorted. This work was supported by NSF grant AST065738 and NASA grants NNX08AH44G, NNX07AH79G and NNX07AO71G. The simulations were performed at the NASA Advanced Supercomputing Division of the Ames Research Center.

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