Buoyant magnetic flux tubes in supergranules

Details Buoyant magnetic flux tubes in supergranules Buoyant magnetic flux tubes in supergranules

Jun 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979a%26a....76...35m&link_type=abstract

Astronomy and Astrophysics, vol. 76, no. 1, June 1979, p. 35-45.

Physics

21

Dynamo Theory, Magnetic Flux, Solar Granulation, Solar Magnetic Field, Aerodynamic Drag, Atmospheric Models, Buoyancy, Graphs (Charts), Kinematics, Lorentz Force, Magnetic Field Configurations, Photosphere, Solar Physics, Sunspots

Scientific paper

The motion of filamentary flux tubes is described by a simplified model. Relative to the prescribed supergranular flow, the tubes drift at a rate determined by magnetic buoyancy, Lorentz forces and aerodynamic drag. The effect of buoyancy is most pronounced near the surface: small flux tubes are swept towards the network at the edge of a cell but those with larger fluxes float vertically at the center. New flux emerges at the center of the cell. These results are related to the emergence of active regions and ephemeral active regions, and to the slow decay of sunspots.

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