Solar Magneto-Convection Simulations of Emergin Flux

Details Solar Magneto-Convection Simulations of Emergin Flux Solar Magneto-Convection Simulations of Emergin Flux

Dec 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009agufmsh11b..05s&link_type=abstract

American Geophysical Union, Fall Meeting 2009, abstract #SH11B-05

Astronomy and Astrophysics

Astrophysics

[7522] Solar Physics, Astrophysics, And Astronomy / Helioseismology, [7524] Solar Physics, Astrophysics, And Astronomy / Magnetic Fields, [7544] Solar Physics, Astrophysics, And Astronomy / Stellar Interiors And Dynamo Theory

Scientific paper

We present preliminary results of magneto-convection simulations of the rise of initially horizontal magnetic flux from 20 Mm deep through the solar surface in a domain 48 Mm wide. 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. Stronger fields rise faster due to magnetic buoyancy (lower density in the strong field region). Slow, large scale, diverging motions sweep the magnetic field to the boundaries of supergranular like structures to form a magnetic network. The field strength varies with depth as the cube root of the density.

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