Solar Magneto-Convection

Details Solar Magneto-Convection Solar Magneto-Convection

Jan 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998aas...191.7417s&link_type=abstract

American Astronomical Society, 191st AAS Meeting, #74.17; Bulletin of the American Astronomical Society, Vol. 29, p.1326

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We present results of realistic simulations of magneto-convection near the solar surface. The simulations were performed with two magnetic field topologies - (1) a unipolar, initially vertical field, and (2) a bipolar field, where fluid entering at the base of the computational domain advects in horizontal field. As the unipolar flux is increased, the magnetic field concentrates in the intergranule lanes and develops large, dark, cool regions. These regions surround smaller areas where convection has not been suppressed. In contrast, for the bipolar case, the strongest fields appear as bright points in the intergranule lanes.

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