Simulation of Flux Emergence in Solar Active Regions

Details Simulation of Flux Emergence in Solar Active Regions Simulation of Flux Emergence in Solar Active Regions

Dec 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufmsh31a1781f&link_type=abstract

American Geophysical Union, Fall Meeting 2010, abstract #SH31A-1781

Astronomy and Astrophysics

Astrophysics

[7524] Solar Physics, Astrophysics, And Astronomy / Magnetic Fields, [7529] Solar Physics, Astrophysics, And Astronomy / Photosphere

Scientific paper

We present results of magnetohydrodynamic (MHD) simulations of magnetic flux emergence from the convection zone into the solar corona using BATSRUS. The MHD equations are modified to take account of the radiative terms, coronal heating and heat conduction. The implementation of non-ideal equation of state describes the partially ionized plasma in the convection zone. The simulations are carried out on a domain of active-region size of 30×30×40 Mm3, extending 20 Mm down into the convection zone. The magnetic fields are coupled with the convective motion during the emerging process, and concentrates in the downflow regions. A coherent shear pattern is formed in the lower corona during the rising. We also compare our model results at the photosphere with SDO/HMI vector magnetograms and illustrate the mechanism of flux emergence that give rise to complexity of the structures in active regions.

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