Convective intensification of magnetic fields at the solar surface.

Details Convective intensification of magnetic fields at the solar surface. Convective intensification of magnetic fields at the solar surface.

Nov 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996nawg.1996..185s&link_type=abstract

Nachr. Akad. Wiss. Göttingen II, Jahrg. 1996, Nr. 4, p. 185 - 192

Physics

Solar Magnetic Fields: Solar Granulation, Solar Magnetic Fields: Solar Convective Zone

Scientific paper

The evolution of an initially homogeneous vertical magnetic field is followed, starting from an evolved state of a 2D numerical simulation of solar granulation. The field is concentrated in the intergranular lane by the combined action of flux expulsion and field intensification by the downflow. A flux sheet forms with a maximum field strength of 1600 G at the solar surface, a value well above the equipartition field strength of about 700 G. The rapid downflow within the flux sheet bounces off the high density plasma in the deeper layers of the flux sheet; the resulting upflow leads to a strong, upward moving shock and to the destruction of the flux sheet after a lifetime of about 200 s.

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