(Los Alamos National Laboratory/Depart. of Phys. and Astron. at Michigan State University, USA)
Holistic MHD-Simulation from the Convection Zone to the Chromosphere
A three-dimensional magnetohydrodynamic simulation of the integral layers from the
convection zone to the chromosphere has been carried out. The simulation represents
magnetoconvection in a quiet network-cell interior. The following preliminary new results
are obtained: The chromospheric magnetic field is very dynamic with a continuous
rearrangement of magnetic flux on a time scale of less than 1 min. Rapidly moving
magnetic filaments (rarely exceeding 40 G) form in the compression zone downstream
and along propagating shock fronts that are present throughout the chromosphere.
The magnetic filaments rapidly move, form, and dissolve with the shock waves. Flux
concentrations strongly expand through the photosphere into a more homogeneous, space
filling chromospheric field. "Canopy fields" form on a granular scale above largely
field-free granule centers leading to a mesh-work of current sheets in a height range
between approximately 400 to 900 km.
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