NSO Workshop #23, Solar MHD: Theory and Observations - a High Spatial Resolution Perspective, Sac Peak, USA, 2005

ASP Conf. Series 354, 345 (2006)

Werner Schaffenberger (Kiepenheuer-Institut für Sonnenphysik, Schöneckstrasse 6, 79104 Freiburg, Germany)
Sven Wedemeyer-Böhm (Kiepenheuer-Institut für Sonnenphysik, Schöneckstrasse 6, 79104 Freiburg, Germany)
Oskar Steiner (Kiepenheuer-Institut für Sonnenphysik, Schöneckstrasse 6, 79104 Freiburg, Germany)
Bernd Freytag (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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