Magnetic buoyancy instabilities in the convective overshoot zone

Details Magnetic buoyancy instabilities in the convective overshoot zone Magnetic buoyancy instabilities in the convective overshoot zone

Nov 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984esasp.220...55h&link_type=abstract

In ESA The Hydromagnetics of the Sun p 55-58 (SEE N85-25091 14-92)

Computer Science

Buoyancy, Magnetic Flux, Solar Magnetic Field, Magnetohydrodynamic Stability, Solar Cycles, Solar Interior, Stellar Cores

Scientific paper

A linear stability analysis for a stratified magnetic layer, incorporating the effects of diffusion, wave motion and rotation was performed to test the proposition that for magnetic flux to be stored in the solar interior for times comparable to the solar cycle, the bulk of the magnetic field must be situated in the overshoot region at the base of the convection zone. Flux loss would then occur when the field becomes unstable to instabilities driven by magnetic buoyancy. Results show that instability occurrence is widespread.

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