On magnetic buoyancy in the convection zone

Details On magnetic buoyancy in the convection zone On magnetic buoyancy in the convection zone

Aug 1976

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1976apj...208..222u&link_type=abstract

Astrophysical Journal, vol. 208, Aug. 15, 1976, pt. 1, p. 222, 223.

Astronomy and Astrophysics

Astrophysics

18

Buoyancy, Convective Flow, Dynamo Theory, Magnetic Flux, Solar Magnetic Field, Eddy Viscosity, Magnetohydrodynamic Flow, Thermodynamic Properties, Turbulent Diffusion

Scientific paper

A magnetic flux tube extending horizontally across a stratified atmosphere with gas pressure and temperature subject to uniform gravitational acceleration is considered. Compression and expansion of the tube are such that field strength is proportional to a power of the density. Turbulent viscosity capable of balancing magnetic buoyancy is defined such that the azimuthal field (100 G) can be retained long enough for the solar dynamo to be effective in the solar convection zone. A magnetic field of 200-300 G may be retained in the convective zone for a half solar cycle (about 10 years). No serious limitations seem to be imposed by magnetic buoyancy on a dynamo operating within the convective zone. Temperature perturbations complicate the problem, but do not invalidate the conclusions.

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