Other
Scientific paper
Feb 1984
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984p%26ss...32..213a&link_type=abstract
Planetary and Space Science (ISSN 0032-0633), vol. 32, Feb. 1984, p. 213-217.
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1
Geomagnetism, Magnetic Field Configurations, Magnetic Flux, Magnetohydrodynamic Flow, Solar Magnetic Field, Solar Terrestrial Interactions, Bipolarity, Convection, Motion Simulation, Photosphere
Scientific paper
Some recent solar observations show that a bipolar magnetic flux in an active region tends to disappear in situ, in less than one solar rotation, without evidence of spreading. This feature is difficult to explain if it is assumed that magnetic buoyancy is the dominant force in controlling dynamics of a magnetic flux tube, since the assumption implies no other force to submerge the tube. These observations may be explained by assuming that a convective motion is the major cause for the formation of an Omega-shaped geometry of the magnetic flux tube, but that the flux tube thus arisen is submerged by the counteracting Lorentz force as the convective motion decays. A two-dimensional MHD simulation method is used to demonstrate this possibility.
Akasofu Syuh-Ichi
Gislason G.
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