Physics
Scientific paper
May 1979
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979soph...62...23a&link_type=abstract
Solar Physics, vol. 62, May 1979, p. 23-50.
Physics
112
Buoyancy, Magnetic Flux, Magnetohydrodynamic Stability, Solar Magnetic Field, Solar Rotation, Stratification, Convective Flow, Gas Flow, Magnetic Diffusion, Magnetostatic Fields, Oscillations, Rotating Fluids, Solar Radiation, Stabilization, Thermal Diffusion
Scientific paper
The instability due to magnetic buoyancy of an isolated flux tube in an electrically conducting perfect gas is considered. Attention is given to doubly diffusive reduction of stratification effects, stabilizing effects of rapid rotation, curvature effects, and certain additional effects of rotation and stratification. An attempt is made to describe applications to the solar radiative interior and convection zone. It is estimated that a 100-G magnetic field displaying a moderate decrease with height at a depth of 30,000 km will take about 10 yr to break up into buoyant flux tubes and that the corresponding time scales at depths of 100,000 and 200,000 km are 1000 and 10,000 yr, respectively.
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